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STS-72 Mission Insignia
| Name of Image |
STS-72 Mission Insignia |
| Date of Image |
1995-05-27 |
| Full Description |
The crew patch of STS-72 depicts the Space Shuttle Endeavour and some of the payloads on the flight. The Japanese satellite, Space Flyer Unit (SFU) is shown in a free-flying configuration with the solar array panels deployed. The inner gold border of the patch represents the SFU's distinct octagonal shape. Endeavour?s rendezvous with and retrieval of SFU at an altitude of approximately 250 nautical miles. The Office of Aeronautics and Space Technology's (OAST) flyer satellite is shown just after release from the Remote Manipulator System (RMS). The OAST satellite was deployed at an altitude of 165 nautical miles. The payload bay contains equipment for the secondary payloads - the Shuttle Laser Altimeter (SLA) and the Shuttle Solar Backscatter Ultraviolet Instrument (SSBUV). There were two space walks planned to test hardware for assembly of the International Space Station. The stars represent the hometowns of the crew members in the United States and Japan. |
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| Description |
*Full Res(984 kB)**High View of Melas* Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from "Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. Credit: NASA/JPL/Arizona State University |
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| Description |
*Full Res (1.3 MB)**Mars Canyon with Los Angeles for Scale* A "Grand Canyon of Mars" slices across the Red Planet near its equator. This canyon -- Valles Marineris, or the Mariner Valley -- is 10 times longer and deeper than Arizona's Grand Canyon, and 20 times wider. As the picture shows, you could drop the whole Los Angeles basin into a small part of Valles Marineris and leave plenty of room to spare. In length, the canyon extends far enough that it could reach across the United States from East Coast to West Coast, while its rim stands more than 25,000 feet high, nearly as tall as Earth's Mount Everest. This scene comes from "Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. Credit: NASA/JPL/Arizona State University |
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Pacific Climate Calm: Image
…
nasa, nasaimageofthedaygalle
…
In early 2006, a weak eartho
…
ssh_jas_2006144
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2006-05-21 |
| creator |
NASA -- Image courtesy NASA/JPL Ocean Surface Topography from Space team |
| identifier |
ssh_jas_2006144 |
|
El Nino May Be Morphing to L
…
nasa, nasaimageofthedaygalle
…
New data of sea level height
…
PIA09208
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2007-02-12 |
| creator |
NASA -- NASA image by JPL sealevel.jpl.nasa.gov/ Ocean Surface Topography Team. |
| identifier |
PIA09208 |
|
Vertical Profile of the Smok
…
nasa, nasaimageofthedaygalle
…
A new instrument in orbit ab
…
GLAS_2003301
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2003-10-28 |
| creator |
NASA -- Image courtesy Steve Palm, https://icesat.gsfc.nasa.gov/ ICESat Team, NASA Goddard Space Flight Center |
| identifier |
GLAS_2003301 |
|
TOPEX/El Niño Watch - June 2
…
PIA00735
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - June 25, 1997 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S./French TOPEX/POSEIDON satellite. The image shows sea surface height relative to normal ocean conditions on June 25, 1997 and provides more convincing information that the weather-disrupting phenomenon known as El Niño is back and getting stronger. The white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it s about 10 centimeters (4 inches) above normal. The surface area covered by the warm water mass is about one and one-half times the size of the continental United States. The added amount of oceanic warm water near the Americas, with a temperature between 21-30 degrees Celsius (70-85 degrees Fahrenheit), is about 30 times the volume of water in all the U.S. Great Lakes combined. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmosphere system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration, (NOAA), has issued an advisory indicating the presence of the early indications of El Niño conditions. |
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TOPEX/El Niño Watch - March
…
PIA00734
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - March thru June, 1997 |
| Original Caption Released with Image |
These four views of the Pacific Ocean were produced using sea surface height measurements taken by the U.S./French TOPEX/POSEIDON satellite. The images show sea surface height relative to normal ocean conditions from March 1997 through June 1997. This evolutionary view is providing oceanographers with more convincing information that the weather-disrupting phenomenon known as El Niño is back and getting stronger. The white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it s about 10 centimeters (4 inches) above normal. The surface area covered by the warm water mass is about one and one-half times the size of the continental United States. The added amount of oceanic warm water near the Americas, with a temperature between 21-30 degrees Celsius (70-85 degrees Fahrenheit), is about 30 times the volume of water in all the U.S. Great Lakes combined. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmosphere system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration, (NOAA), has issued an advisory indicating the presence of the early indications of El Niño conditions. |
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TOPEX/El Niño Watch - Octobe
…
PIA00741
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - October 3, 1997 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S./French TOPEX/Poseidon satellite. The image shows sea surface height relative to normal ocean conditions on Oct. 3, 1997 as the warm water associated with El Niño (in white) spreads northward along the entire coast of North America from the equator all the way to Alaska. The warm water pool in tropical Pacific resulting from El Niño seems to have stabilized. The white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The surface area covered by the warm water mass is about one and one-half times the size of the continental United States. The added amount of oceanic warm water near the Americas, with a temperature between 21 and 30 C (70 to 85 F), carries the amount of heat equal to 100 times the amount of fossil fuel energy consumed by the entire U.S. population during one year. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmosphere system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration (NOAA) has issued an advisory indicating the presence of a strong El Niño condition throughout the coming winter. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov/ |
|
TOPEX/El Niño Watch- Septemb
…
PIA00736
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch- September 20, 1997 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S./French TOPEX/POSEIDON satellite. The image shows sea surface height relative to normal ocean conditions on September 20, 1997 and provides more convincing information that the weather-disrupting phenomenon known as El Niño is back and getting stronger. The white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters ( 6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The surface area covered by the warm water mass is about one and one-half times the size of the continental United States. The added amount of oceanic warm water near the Americas, with a temperature between 21-30 degrees Celsius (70-85 degrees Fahrenheit), is about 30 times the volume of water in all the U.S. Great Lakes combined. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmosphere system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration, (NOAA), has issued an advisory indicating the presence of the early indications of El Niño conditions. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov/ |
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TOPEX/El Niño Watch - El Niñ
…
PIA01164
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - El Niño Warm Water Pool Decreasing, Jan, 08, 1998 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S.-French TOPEX/Poseidon satellite. The image shows sea surface height relative to normal ocean conditions on Jan. 8, 1998, and sea surface height is an indicator of the heat content of the ocean. The volume of the warm water pool related to the El Niño has decreased by about 40 percent since its maximum in early November, but the area of the warm water pool is still about one and a half times the size of the continental United States. The volume measurements are computed as the sum of all the sea surface height changes as compared to normal ocean conditions. In addition, the maximum water temperature in the eastern tropical Pacific, as measured by the National Oceanic and Atmospheric Administration (NOAA), is still higher than normal. Until these high temperatures diminish, the El Niño warm water pool still has great potential to disrupt global weather because the high water temperatures directly influence the atmosphere. Oceanographers believe the recent decrease in the size of the warm water pool is a normal part of El Niño's natural rhythm. TOPEX/Poseidon has been tracking these fluctuations of the El Niño warm pool since it began in early 1997. These sea surface height measurements have provided scientists with their first detailed view of how El Niño's warm pool behaves because the TOPEX/Poseidon satellite measures the changing sea surface height with unprecedented precision. In this image, the white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmosphere system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration, (NOAA), has issued an advisory indicating the presence of a strong El Niño condition throughout the winter. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov |
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Phyllosilicate and Olivine a
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PIA09933
Sol (our sun)
CRISM
| Title |
Phyllosilicate and Olivine around a Fracture in Nili Fossae |
| Original Caption Released with Image |
The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) took this observation of part of the Nili Fossae region at the western margin of the Isidis impact basin at 3:07 (UTC) on December 12, 2006, near 21.9 degrees north latitude, 78.2 degrees east longitude. The image was taken in 544 colors covering 0.36-3.92 micrometers, and shows features as small as 18 meters (60 feet) across. The image is about 11 kilometers (7 miles) wide at its narrowest point. The Isidis basin resulted from a gigantic impact on the surface of Mars early in the planet's history. The image of the Isidis basin at the top left is the colored elevation data from the Mars Orbiter Laser Altimeter (MOLA) overlain on a digital image mosaic from the Viking mission. Reds represent higher elevations, and blue lower elevations. The western rim of the Isidis basin has numerous, concentric troughs (or "fossae") which may have formed during faulting associated with the impact event. Since then, the Nili Fossae region has since been heavily eroded, and is one of the most mineralogically diverse spots on Mars. This CRISM image targets one of region's smaller fractures. The image is shown overlain on the Viking digital image mosaic at lower left. The lower right CRISM image was constructed from three visible wavelengths (0.71, 0.60 and 0.53 microns in the red, green and blue image planes, respectively) and is close to what the human eye would see. The blue on the right of the image is an artifact from light scattering in the atmosphere. The upper right image was constructed from three infrared channels (2.38, 1.80 and 1.15 microns in the red, green and blue image planes, respectively) to highlight the mineralogy of the area. The bright green areas are rich in "phyllosilicates," a category of minerals including clays. The purple material along the walls of the fracture likely contains small amounts of the iron- and magnesium-rich mineral pyroxene. The yellow-brown material contains the iron- and magnesium-rich mineral olivine. Olivine and pyroxene are minerals associated with igneous activity. Overlaying CRISM data with images from the High-Resolution Imaging Science Experiment (HiRISE) camera shows that the phyllosilicates are in small, eroded outcrops of rock. The olivine is most abundant in sand dunes on the surface. The use of these two instruments together reveals more about the history of the region: Olivine sands covered the area shown in the image after the interaction of water and rock formed the phyllosilicates and after the fracture formed. The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is one of six science instruments on NASA's Mars Reconnaissance Orbiter. Led by The Johns Hopkins University Applied Physics Laboratory, the CRISM team includes expertise from universities, government agencies and small businesses in the United States and abroad. |
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TOPEX/El Niño Watch - El Niñ
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PIA01451
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - El Niño is Still Lingering in the Pacific May 3, 1998 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea-surface height measurements taken by the U.S.-French TOPEX/Poseidon satellite. The image shows sea-surface height relative to normal ocean conditions on May 3, 1998, and sea-surface height is an indicator of the heat content of the ocean. The image shows that sea-surface height along the central and eastern equatorial Pacific has maintained a near normal state since March 1998. However, the western equatorial Pacific, shown here in purple, has not returned to a normal state and is still about 30 centimeters (12 inches) below normal sea level. Remnants of the El Niño warm water pool, shown in red and white, are situated to the north of the equator. Oceanographers indicate these measurements show that the Pacific has not yet fully recovered from this large El Niño event. These sea-surface height measurements have provided scientists with a detailed view of how the 1997-98 El Niño's warm water pool behaves because the TOPEX/Poseidon satellite measures the changing sea-surface height with unprecedented precision. In this image, the white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The green areas indicate normal conditions. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using satellite imagery, buoy and ship data, and a forecasting model of the ocean-atmosphere system, the National Oceanic and Atmospheric Administration, (NOAA), has continued to issue an advisory indicating the so-called El Niño weather conditions that have impacted much of the United States and the world are expected to remain through the spring. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov |
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TOPEX/El Niño Watch - Warm W
…
PIA01448
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - Warm Water Pool is Thinning, Feb, 5, 1998 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S.-French TOPEX/Poseidon satellite. The image shows sea surface height relative to normal ocean conditions on Feb. 5, 1998 and sea surface height is an indicator of the heat content of the ocean. The area and volume of the El Niño warm water pool that is affecting global weather patterns remains extremely large, but the pool has thinned along the equator and near the coast of South America. This "thinning" means that the warm water is not as deep as it was a few months ago. Oceanographers indicate this is a classic pattern, typical of a mature El Niño condition that they would expect to see during the ocean's gradual transition back to normal sea level. In this image, the white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using satellite imagery, buoy and ship data, and a forecasting model of the ocean-atmosphere system, the National Oceanic and Atmospheric Administration, (NOAA), has continued to issue an advisory indicating the so-called El Niño weather conditions that have impacted much of the United States and the world are expected to remain through the spring. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov |
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TOPEX/El Niño Watch - Satell
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PIA01449
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - Satellite shows El Niño-related Sea Surface Height, Mar, 14, 1998 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S.-French TOPEX/Poseidon satellite. The image shows sea surface height relative to normal ocean conditions on Mar. 14, 1998 and sea surface height is an indicator of the heat content of the ocean. The image shows that the sea surface height along the central equatorial Pacific has returned to a near normal state. Oceanographers indicate this is a classic pattern, typical of a mature El Niño condition. Remnants of the El Niño warm water pool, shown in red and white, are situated to the north and south of the equator. These sea surface height measurements have provided scientists with a detailed view of how the 1997-98 El Niño's warm pool behaves because the TOPEX/Poseidon satellite measures the changing sea surface height with unprecedented precision. In this image, the white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using satellite imagery, buoy and ship data, and a forecasting model of the ocean-atmosphere system, the National Oceanic and Atmospheric Administration, (NOAA), has continued to issue an advisory indicating the so-called El Niño weather conditions that have impacted much of the United States and the world are expected to remain through the spring. |
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TOPEX/El Niño Watch - Strong
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PIA02935
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - Strong, Long-lasting La Niña Just Fading Away, June 19, 2000 |
| Original Caption Released with Image |
."Let's not forget that the legacy of two years of La Niña will be with us this summer and into the fall," said JPL oceanographer Dr. William Patzert. "Much of the nation's farmland is really dry in many regions. The reality is that the atmosphere is still acting as though La Niña remains." The National Oceanic and Atmospheric Administration's (NOAA) National Weather Service has forecasted continuing drought for much of the midwestern and southeastern United States and an active hurricane season for our coming summer. NOAA seasonal forecasts can be found at http://www.cpc.ncep.noaa.gov [ http://www.cpc.ncep.noaa.gov ] . The U.S.-French TOPEX/Poseidon mission is managed by JPL for the NASA's Earth Science Enterprise, Washington, D.C. JPL is a division of the California Institute of Technology in Pasadena. For more information on the TOPEX/Poseidon project, see http://topex-www.jpl.nasa.gov [ http://topex-www.jpl.nasa.gov ], After dominating the tropical Pacific Ocean for more than two years, the 1998-2000 La Niña "cool pool" is continuing its slow fade and seems to be retiring from the climate stage, according to the latest satellite data from the U.S.-French TOPEX/Poseidon mission. These data, taken during a 10-day cycle of collection ending June 9, show that the equatorial Pacific continues to warm up and is returning to normal (green) as this latest, persistent, two-year La Niña episode is coming to an end. Only a few patches of cooler, lower sea levels (seen in blue and purple) remain across the tropics. It should be noted that in June 1999, La Niña barely had a pulse, but was resuscitated in fall 1999. (See June 1999 press release on that topic at http://www.jpl.nasa.gov/elnino/990629.html [ http://www.jpl.nasa.gov/elnino/990629.html ] .) The blue areas are between 5 and 13 centimeters (2 and 5 inches) below normal, whereas the purple areas range from 14 to 18 centimeters (6 to 7 inches) below normal. In the far-western tropical Pacific Ocean, the ocean remains higher and warmer than normal. In summary, it appears that the global climate system is finally emerging from the past three years of dramatic swings from the extra-large El Niño of 1997/1998, which was followed by two unusually cool and persistent La Niña years, according to scientists at NASA's Jet Propulsion Laboratory. But as the northern hemisphere summer begins, above-normal sea surface heights and warmer ocean temperatures (indicated by the red and white areas) still blanket the western equatorial Pacific and much of the north and south mid-Pacific. Red areas are about 10 centimeters (4 inches) above normal, white areas show the sea surface height is between 14 and 32 centimeters (6 to 13 inches) above normal. This contrasts with the Bering Sea and Gulf of Alaska region southward along the western coast of North America, where lower-than-normal sea levels and cool ocean temperatures continue, although this pattern is also weakening. A possible switch in this larger-than-El Niño/La Niña, slower-changing pattern -- the Pacific Decadal Oscillation -- was first noticed by many scientists in late 1998. See a January 2000 press release on that topic at http://www.jpl.nasa.gov/elnino/20000118.html [ http://www.jpl.nasa.gov/elnino/20000118.html ] , or for further information and graphics about the Pacific Decadal Oscillation, see http://topex-www.jpl.nasa.gov/discover/PDO.html [ http://topex-www.jpl.nasa.gov/discover/PDO.html ] |
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TOPEX/El Niño Watch - Los Ni
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PIA02969
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - Los Niños may be Gone, But Pacific Pattern Remains August 14, 2000 |
| Original Caption Released with Image |
After three years of El Niño and La Niña with their often devastating climate consequences, the Pacific is finally calming down in the tropics but still shows signs of being abnormal elsewhere, according to the latest satellite data from the U.S.-French TOPEX/Poseidon mission. These data, taken during a 10-day cycle of collection ending August 17, show that tropical Pacific sea levels, which indicate how much heat is stored in the ocean, have returned to near-normal (green) after three years of dramatic fluctuations. See http://www.jpl.nasa.gov/elnino/ . But as summer ends in the Northern Hemisphere, remnants of the past few years remain embedded in the upper ocean. Above-normal sea surface heights and warmer ocean temperatures (indicated by the red and white areas) still blanket the far-western tropical Pacific and much of the north (and south) mid-Pacific. Red areas are about 10 centimeters (4 inches) above normal, white areas show the sea surface height is between 14 and 32 centimeters (6 to 13 inches) above normal. This contrasts with the Bering Sea and Gulf of Alaska where lower-than-normal sea levels and cool ocean temperatures continue (indicated by blue areas), although this pattern is also weakening. The blue areas are between 5 and 13 centimeters (2 and 5 inches) below normal, whereas the purple areas range from 14 to 18 centimeters (6 to 7 inches) below normal. Looking at the entire Pacific basin, the Pacific Decadal Oscillation's (PDO) characteristic warm horseshoe and cool wedge pattern is still evident in this sea-level height image. The PDO is a long-term ocean temperature fluctuation of the Pacific Ocean that waxes and wanes approximately every 10 to 20 years. Most recent National Oceanic and Atmospheric Administration (NOAA) sea-surface temperature date also clearly illustrate the persistence of this basin-wide pattern. They are available at: http://psbsgi1.nesdis.noaa.gov:8080/PSB/EPS/SST/climo.html."The present calming started three to four months ago when the La Niña faded away," said oceanographer Dr. William Patzert of NASA's Jet Propulsion Laboratory, Pasadena, Calif. "It appears that the global climate system is finally recovering from the past three years of dramatic swings from the extra-large El Niño of 1997/1998, which was followed by two unusually cool and persistent La Niña years.""The good news is that we're finally out from under the El Niño and La Niña of the past three years," Patzert said. "Unfortunately, in the longer term, the reality is that the PDO pattern still dominates the Pacific and, in the short term, the atmosphere is still acting as though La Niña remains. The western United States continues hot and dry, and a larger than normal number of hurricanes are forecast by NOAA for both the Pacific and the Atlantic. Also for the remainder of the summer and into the fall, we are continuing to experience the legacy or hangover from El Niño and La Niña -- the devastating Western U.S. fires from the, Canadian to Mexican borders are one example." National Oceanic and Atmospheric Administration's (NOAA) National Weather Service has forecasted continuing heat in the Western United States and an active hurricane season for the end of summer and into the fall. NOAA seasonal forecasts can be found at: http://www.cpc.ncep.noaa.gov. This month marks the eighth anniversary of the launch of TOPEX/Poseidon, a mission that had been planned to last only three to five years. The satellite has orbited Earth more than 37,400 times and completed 290 10-day data collection cycles. More than 99 percent of all available mission data has been collected and archived by the operations team at JPL. The U.S.-French TOPEX/Poseidon mission is managed by JPL for the NASA's Earth Science Enterprise, Washington, D.C. JPL is a division of the California Institute of Technology in Pasadena. For more information on the TOPEX/Poseidon project, see http://topex-www.jpl.nasa.gov [ http://topex-www.jpl.nasa.gov ] |
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Pacific Shows Signs of Morph
…
PIA09208
Sol (our sun)
Altimeter
| Title |
Pacific Shows Signs of Morphing From Warm El Nino To Cool La Nina |
| Original Caption Released with Image |
New data of sea-level heights from early February, 2007, by the Jason altimetric satellite show that the tropical Pacific Ocean has transitioned from a warm (El Niño) to a cool (La Niña) condition during the prior two months. The beginnings of a possible La Niña are indicated by the blue area (in the center of the image along the equator) of lower than normal sea level (cold water). It is not certain yet if this current cooling trend will eventually evolve into a long-lasting, well-developed La Niña. "La Niña could send an already parched Western United States to its knees," said JPL oceanographer Dr. Bill Patzert. "In the Southwest, we call La Niña the little lady with the big dry punch." A La Niña situation often follows an El Niño episode and is essentially the opposite of an El Niño condition. During a La Nina, trade winds are stronger than normal, and the cold water that normally exists along the coast of South America extends to the central equatorial Pacific. A La Niña situation changes global weather patterns and is associated with less moisture in the air, resulting in less rain along the coasts of North and South America. Jason will continue to track this developing switch in the climate. This image of the Pacific Ocean was produced using sea-surface height measurements taken by the U.S.-French Jason satellite. The image is based on the average of 10 days of data centered on February 12, 2007, compared to the long-term average of observations from 1993 through 2005. In this image, places where the Pacific sea surface height is higher (warmer) than normal are yellow and red, and places where the sea surface is lower (cooler) than normal are blue and purple. Green shows where conditions are near normal. Sea-surface height is an indicator of the heat content of the upper ocean. NASA's Jet Propulsion Laboratory manages the U.S. portion of the U.S./French Jason mission for NASA's Science Mission Directorate, Washington, D.C. JPL is a division of the California Institute of Technology, Pasadena, Calif. For more information on NASA's ocean surface topography missions, see http://sealevel.jpl.nasa.gov/ [ http://sealevel.jpl.nasa.gov/ ] or to view the latest Jason data see http://sealevel.jpl.nasa.gov/science/jason1-quick-look/ [ http://sealevel.jpl.nasa.gov/science/jason1-quick-look/ ]. |
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High View of Melas
PIA02893
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
High View of Melas |
| Original Caption Released with Image |
Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
|
High View of Melas
PIA02893
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
High View of Melas |
| Original Caption Released with Image |
Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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High View of Melas
PIA02893
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
High View of Melas |
| Original Caption Released with Image |
Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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High View of Melas
PIA02893
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
High View of Melas |
| Original Caption Released with Image |
Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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High View of Melas
PIA02893
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
High View of Melas |
| Original Caption Released with Image |
Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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High View of Melas
PIA02893
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
High View of Melas |
| Original Caption Released with Image |
Soaring high above Valles Marineris, the "Grand Canyon of Mars," viewers look down and catch a sight resembling parts of the desert West of the United States, but on a vastly greater scale. Here the canyon averages over a hundred miles wide, and its floor is heaped with rocks, sediments, and landslide debris. Within the canyon walls lie possibly hundreds of layers filling many pages of Mars' geologic record. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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Mars Canyon with Los Angeles
…
PIA02891
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Mars Canyon with Los Angeles for Scale |
| Original Caption Released with Image |
A "Grand Canyon of Mars" slices across the Red Planet near its equator. This canyon -- Valles Marineris, or the Mariner Valley -- is 10 times longer and deeper than Arizona's Grand Canyon, and 20 times wider. As the picture shows, you could drop the whole Los Angeles basin into a small part of Valles Marineris and leave plenty of room to spare. In length, the canyon extends far enough that it could reach across the United States from East Coast to West Coast, while its rim stands more than 25,000 feet high, nearly as tall as Earth's Mount Everest. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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Mars Canyon with Los Angeles
…
PIA02891
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Mars Canyon with Los Angeles for Scale |
| Original Caption Released with Image |
A "Grand Canyon of Mars" slices across the Red Planet near its equator. This canyon -- Valles Marineris, or the Mariner Valley -- is 10 times longer and deeper than Arizona's Grand Canyon, and 20 times wider. As the picture shows, you could drop the whole Los Angeles basin into a small part of Valles Marineris and leave plenty of room to spare. In length, the canyon extends far enough that it could reach across the United States from East Coast to West Coast, while its rim stands more than 25,000 feet high, nearly as tall as Earth's Mount Everest. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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Mars Canyon with Los Angeles
…
PIA02891
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Mars Canyon with Los Angeles for Scale |
| Original Caption Released with Image |
A "Grand Canyon of Mars" slices across the Red Planet near its equator. This canyon -- Valles Marineris, or the Mariner Valley -- is 10 times longer and deeper than Arizona's Grand Canyon, and 20 times wider. As the picture shows, you could drop the whole Los Angeles basin into a small part of Valles Marineris and leave plenty of room to spare. In length, the canyon extends far enough that it could reach across the United States from East Coast to West Coast, while its rim stands more than 25,000 feet high, nearly as tall as Earth's Mount Everest. This scene comes from """Flight Through Mariner Valley," an exciting video produced for NASA by the Jet Propulsion Laboratory. The video takes viewers on a simulated flight into Valles Marineris, where they explore its scenic wonders as their imaginary scout ship dives low over landslides and races through winding canyons. The video features high-resolution images from Arizona State University's Thermal Emission Imaging System multi-band camera on NASA's Mars Odyssey. The images, which show details as small as 300 meters (1,000 feet) across, were taken at infrared wavelengths during the Martian daytime. Scientists joined hundreds of individual frames from the camera into a giant mosaic, then colored the mosaic to approximate how Mars would appear to the human eye. To give the mosaic depth and height, moviemakers fitted it to a computerized topographic model for Valles Marineris. This was developed using hundreds of thousands of altitude measurements by the Mars Orbiter Laser Altimeter, an instrument on NASA's Mars Global Surveyor spacecraft. |
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3000 Mile Laser Altimeter Pr
…
PIA00958
Sol (our sun)
MOLA
| Title |
3000 Mile Laser Altimeter Profile Across Northern Hemisphere of Mars |
| Original Caption Released with Image |
Topographic profile across the northern hemisphere of Mars from the Mars Orbiter Laser Altimeter (MOLA). The profile was obtained during the Mars Global Surveyor Capture Orbit Calibration Pass on September 15, 1997 and represents 20 minutes of data collection. The profile has a length of approximately 3000 miles (5000 kilometers). The large bulge is the western part of the Elysium rise, the second largest volcanic province on Mars, and shows over 3 miles (5 kilometers) of vertical relief. This area contains deep chasms that reflect tectonic, volcanic and erosional processes. In contrast is the almost 1featureless1 northern plains region of Mars, which shows only hundreds of meters of relief at scales the size of the United States. Plotted for comparison is the elevation of the Viking Lander 2 site, which is located 275 miles (445 kilometers) west of the profile. At the southernmost extent of the trace is the transition from the northern plains to the ancient southern highlands. Characterizing the fine-scale nature of topography in this chaotic region is crucial to testing theories for how the dichotomy between the geologically distinctive northern lowlands and southern uplands formed and subsequently evolved. The spatial resolution of the profile is approximately 1000 feet (330 meters) and the vertical resolution is approximately 3 feet (1 meter). When the Mars Global Surveyor mapping mission commences in March, 1998, the MOLA instrument will collect 72 times as much data every day for a period of two years. |
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TOPEX/El Niño Watch - Octobe
…
PIA01053
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - October 23, 1997 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S./French TOPEX/POSEIDON satellite. The image shows sea surface height relative to normal ocean conditions on Oct. 23, 1997 as the warm water associated with El Niño (in white) spreads northward along the entire coast of North America from the equator all the way to Alaska. The warm water pool associated with the El Niño has returned to the volume it was in mid-September after dropping to a temporary low at the beginning of October. The sea surface elevation just north of the El Niño warm pool continues to drop (purple area), enhancing the eastward flowing North Equatorial Counter Current. The intensification of this current is another tell-tale sign of the El Niño phenomenon. This flow contributes to the rise in sea level along the western coasts of the Americas that will progress towards both the north and south poles over the next several months. The white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The surface area covered by the warm water mass is about one and one-half times the size of the continental United States. The added amount of oceanic warm water near the Americas, with a temperature between 21-30 degrees Celsius (70- 85 degrees Fahrenheit), is about 30 times the volume of water in all the U.S. Great Lakes combined. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmosphere system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration, (NOAA), has issued an advisory indicating the presence of a strong El Niño condition throughout the winter. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov/ |
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TOPEX/El Niño Watch - Warm W
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PIA01085
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - Warm Water Pool is Increasing, Nov. 10, 1997 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S./French TOPEX/Poseidon satellite. The image shows sea surface height relative to normal ocean conditions on Nov. 10, 1997. The volume of extra warm surface water (shown in white) in the core of the El Niño continues to increase, especially in the area between 15 degrees south latitude and 15 degrees north latitude in the eastern Pacific Ocean. The area of low sea level (shown in purple) has decreased somewhat from late October. The white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 centimeters and 32 cm (6 inches to 13 inches) above normal, in the red areas, it is about 10 centimeters (4 inches) above normal. The surface area covered by the warm water mass is about one-and-one-half times the size of the continental United States. The added amount of oceanic warm water near the Americas, with a temperature between 21 to 30 degrees Celsius (70 to 85 degrees Fahrenheit), is about 30 times the volume of water in all the U.S. Great Lakes combined. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white areas) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using these global data, limited regional measurements from buoys and ships, and a forecasting model of the ocean-atmospheric system, the National Centers for Environmental Prediction (NCEP) of the National Oceanic and Atmospheric Administration (NOAA) has issued an advisory indicating the presence of a strong El Niño condition throughout the winter. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov/ |
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Jason Satellite Observes Mil
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PIA01939
Sol (our sun)
Altimeter
| Title |
Jason Satellite Observes Mild El Nino in 2006 |
| Original Caption Released with Image |
In September 2006, NASA satellite data indicated that El Niño had returned to the tropical Pacific Ocean, although it was relatively weak. As of early October, scientists were not sure if the event would persist, and it was much less intense than the last major El Niño episode, which happened in 1997-1998. That event brought devastating floods to California that cost millions of dollars in damage while severe drought struck Indonesia, Australia, and the Philippines. Among the ocean characteristics that signal developing El Niño events is a change in average sea surface height compared to normal sea level. When water warms, it expands a little, which changes its volume slightly. When heat begins to build up in the Pacific during an El Niño event, the sea surface height begins to creep up. NASA observes changes in average sea surface height using its Jason satellite. The image is based on the average of 10 days of data centered on September 15, 2006, compared to the long-term average of observations from 1993-2005. In this image, places where the Pacific sea surface height is higher (warmer) than normal are yellow, orange, and red, and places where the sea surface is lower (cooler) than normal are blue and purple. Green shows where conditions are near normal. The swath of red in the center of the scene reveals that an El Niño was in progress when Jason observed the Pacific. El Niño is a cyclical warming of the ocean waters in the central and eastern tropical Pacific that generally occurs every 3 to 7 years. It is linked with changes in air pressure and high-level winds that can affect weather worldwide. Typically peaking during the Northern Hemisphere winter months, El Niño is the warm phase of the El Niño/Southern Oscillation. It alternates with La Niña, the cooling of ocean waters in the same region of the Pacific. According to Bill Patzert, oceanographer and climatologist at NASA's Jet Propulsion Laboratory, "The present conditions indicate that the intensity of this El Niño is too weak to have a major influence on current weather patterns. But, if the ocean waters continue to warm and spread eastward, this event would likely strengthen, perhaps bringing much-needed rainfall to the southwestern and southeastern United States this winter." The Jason satellite carries a dual-frequency radar altimeter. This instrument beams microwave pulses-at 13.6 and 5.3 Gigahertz, respectively-downward toward the Earth. To determine the ocean's height, the instrument precisely measures the time it takes for the microwave pulses to bounce off the surface and return to the spacecraft. This measure, multiplied by the speed of light, gives the range from the satellite to the ocean surface. The joint U.S.-French Topex/Poseidon mission is managed by the JPL for NASA's Science Mission Directorate, NASA Headquarters, Washington, D.C. JPL is a division of the California Institute of Technology in Pasadena. Research on Earth's oceans using Jason and other, space-based capabilities is conducted by NASA's Science Mission Directorate to better understand and protect our home planet. For more information on NASA's ocean surface topography missions, see http://sealevel.jpl.nasa.gov/ [ http://sealevel.jpl.nasa.gov/ ] or to view the latest Jason data see http://sealevel.jpl.nasa.gov/science/jason1-quick-look/ [ http://sealevel.jpl.nasa.gov/science/jason1-quick-look/ ]. |
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Procedure for Finding New Im
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PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
Procedure for Finding New Im
…
PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
Procedure for Finding New Im
…
PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
Procedure for Finding New Im
…
PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
Procedure for Finding New Im
…
PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
Procedure for Finding New Im
…
PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
Procedure for Finding New Im
…
PIA09021
Sol (our sun)
Mars Orbiter Camera
| Title |
Procedure for Finding New Impact Sites on Mars Using the Mars Global Surveyor Mars Orbiter Camera |
| Original Caption Released with Image |
), the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) science operations team considered it possible to find more such impact sites using the MOC red wide angle camera. The most recent, freshest craters would be expected to be quite small, ranging from a few meters across to maybe a few hundred meters or so, at most, in diameter (100 meters is about 109 yards, compare that with a 100 yard U.S.-style football field). Something less than 100 meters across would not show up easily in a 240 meters per pixel red wide angle image. But the 6 January 2006 image showed that it could, because these small impacts, if they occur in an area thickly mantled with dust, will create a much larger "blast zone" around them. Thus, the MOC science operations team set out to image a few of the dustiest regions on Mars -- Tharsis, Amazonis, and Arabia -- with the red wide angle camera. The same camera had, in May and early June 1999, already imaged most of the planet at about 240 meters per pixel scale. By repeating areas already imaged in May/June 1999 during the January/March 2006 timeframe, we would be able to identify more dark spots. And, so, that is what we did. The Tharsis, Amazonis, and Arabia regions were re-imaged using the MOC red wide angle camera during January through March 2006. The data covered about 21,506,000 square kilometers (~8.3 million square miles, ~1/3 the surface area of Mars and more than twice the area of the United States). As each picture was received on Earth, we compared it with the images acquired during May/June 1999. Over the entire area surveyed, we found 39 dark spots that were present in early 2006 but not visible in May/June 1999. The 39 dark spots, then, were the candidate impact sites. Each one of these became a target for the MOC narrow angle camera, which would be used to take an image of about 1.5 meters (4.9 feet) per pixel of each site. The targets were entered into the MOC database. Then, as the predicted MGS ground track came near each site, the MOC team targeted an image by working with the spacecraft engineers at Lockheed Martin Astronautics (Denver, Colorado) and the Caltech/Jet Propulsion Laboratory (JPL, Pasadena, California) to point the spacecraft and camera at each site using the Roll Only Targeted Observation (ROTO) maneuver. Of the 39 dark spots, 20 turned out to be fresh impact sites, and 19 of them were not. The other 19 included mistaken identifications (one was a transient, large dust devil shadow, several were craters that had been present in earlier images but had changed in brightness owing to dust removal), new dark wind streaks, and new dark slope streaks created by avalanching dust on steep slopes. Some of the 20 new impact sites received further attention, as the spacecraft and MOC were used to obtain cPROTO (compensated Pitch and Roll Targeted Observations) views that have a spatial resolution of 0.5 meters (1.6 feet) in the downtrack dimension and 1.5 meters (4.9 feet) in the cross, Having realized that a new dark spot on Mars, seen in a red wide angle camera image acquired on 6 January 2006, might be an indication of a recent meteor impact site (see PIA09020 [ http://photojournal.jpl.nasa.gov/catalog/PIA09020 ] or MOC2-1611 [ http://www.msss.com/mars_images/moc/2006/12/06/craters/site1/index.html ], track direction. The cPROTO views, where obtained, have a higher resolution and better signal-to-noise ratio than the original ROTO images. Finally, while our approach of comparing MOC red wide angle camera images obtained in May/June 1999 with those obtained in January/March 2006 constrains the 20 craters all to having formed during the May 1999 to March 2006 time interval, we found in all cases that there were already other images that had been received on Earth that helped constrain the time of the impact more tightly. In some cases, the date of the impact could be pinned down to within a month or two, in other cases the interval covered several years. Data from the MGS MOC, Mars Odyssey Thermal Emission Imaging System (THEMIS) [ http://themis.asu.edu/ ], and Mars Express High Resolution Stereo Camera (HRSC) [ http://berlinadmin.dlr.de/Missions/express/indexeng.shtml ], were all employed in the search. Shown on this page (above) are pictures that illustrate our work to find new impact craters: Figure A: This picture shows one of the new impact sites identified by the MOC team. Located in northern Arabia Terra near 29.3°N, 333.2°W, the actual crater is quite small, only 11.2 ± 3.0 meters in diameter. This is a sub-frame of MOC image S16-01105, acquired using a ROTO maneuver on 12 March 2006. Figures B and C: These pictures are MOC red wide angle camera images, obtained at a scale of about 240 meters per pixel, of portions of Arabia Terra. Figure B is M01-01610 and was acquired during the MOC Geodesy Campaign (see PIA02022 and PIA02023, or MOC2-127) on 14 May 1999. Figure C, MOC S14-02741, was obtained on 26 January 2006 as part of the campaign to find new impact craters. By comparing the two images, one from 1999 and one from 2006, we were able to identify all new dark spots that formed during that interval. In this case, the new dark spot seen in the 2006 image, S14-02741, is inside the white circle. The same location is also indicated by a circle in the May 1999 image, but no dark spot is present there. In both cases, the white circle is about 12 km (7.5 mi) across. Figure D: This map of Mars, showing the location of all the MOC red wide angle camera images acquired for the search for new craters during January through March 2006. These images cover most of Amazonis, Tharsis, and Arabia Terra. The base map is a product that combines the May/June 1999 MOC red wide angle data (plus later data for the south polar region) and laser altimeter data from MGS. Figure E: This picture shows portions of two red wide angle camera context images that more tightly constrain when the new crater shown here (above, top, left) formed. The first picture, R05-00427, was acquired on 5 May 2003 and shows no dark spot at the site of the impact. The second picture, S05-01885, shows that the dark spot was present on 29 April 2005. Thus, these two images tell us that the impact occurred sometime between those dates: 5 May 2003 and 29 April 2005. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
|
TOPEX/El Niño Watch - La Niñ
…
PIA02436
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - La Niña Conditions Likely to Prevail, October 10, 1999 |
| Original Caption Released with Image |
A repeat of last year's mild La Niña conditions -- with a stormy winter in the Pacific Northwest and a dry winter in the southwestern United States -- will be the likely outcome of sea-surface heights observed by NASA's TOPEX/Poseidon satellite, scientists say. TOPEX/Poseidon has detected lower than normal sea-surface heights in the eastern North Pacific and unusually high sea-surface heights in the western and mid-latitude Pacific. The height of the sea surface over a given area is an indicator of ocean temperature and other factors that influence climate. The latest measurements, taken during a 10-day data cycle October 5-15, are available at http://www.jpl.nasa.gov/elnino . Sea-surface height is shown relative to normal (green) and reveals cooler water (blue and purple) measuring about 14 centimeters (6 inches) lower in the eastern North Pacific, from the Gulf of Alaska to central Alaska, and along the equator. The cooling trend sets the stage for another La Niña this winter."A mirror image of that oceanic profile prevails in the western and mid-latitude Pacific Ocean, where higher than normal sea-surface heights (red and white) are currently about 20 centimeters or 8 inches. Unusually warm temperatures (shown in red and white) have persisted and topped last year's temperatures," said Dr. William Patzert, an oceanographer at NASA's Jet Propulsion Laboratory, Pasadena, CA."These unbalanced conditions will undoubtedly exert a very strong influence on climate over North America this fall and winter," Patzert said. "Our profile of high sea-surface heights and warm temperatures in the western Pacific Ocean contrasts with low sea-surface heights and cool conditions in the eastern and equatorial Pacific. Those conditions will have a powerful impact on the weather system delivering jet streams out of the North Pacific." Conditions are ripe for a stormy, wet winter in the Pacific Northwest and a dry, relatively rainless winter in Southern California and the Southwest, the data show. "Clearly, these unusual conditions, which have persisted for 2 1/2 years, will not be returning to normal any time soon," Patzert said. "This climate imbalance is big and we're definitely going through a decade of wild climatic behavior. But when we look back at the climate record over the past century, we've seen behavior like this before." The TOPEX/Poseidon satellite's measurements have provided scientists with a detailed view of the 1997-1999 El Niño/La Niña climate pattern by measuring the changing sea-surface height with unprecedented precision. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov/ |
|
TOPEX/El Niño Watch - Mild L
…
PIA02437
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - Mild La Niña Conditions Developing, November 12, 1999 |
| Original Caption Released with Image |
Unusually warm ocean temperatures off Asia and cool waters in the eastern and equatorial Pacific are signaling La Niña's mild return, according to the latest sea-surface heights observed by the joint NASA-French space agency's TOPEX/Poseidon satellite. Lower than normal sea-surface heights in the eastern North Pacific and abnormally high sea-surface heights in the western and mid-latitude Pacific are expected to drive storms coming out of the Pacific this winter, the mission data indicate. Those conditions will most likely steer storms north into the Pacific Northwest and keep the southwestern United States dryer than normal. The latest measurements, processed after a 10-day data cycle November 4-13 at NASA's Jet Propulsion Laboratory, Pasadena, CA, are available at http://www.jpl.nasa.gov/elnino . Sea-surface height is shown relative to normal (green) and reveals cooler water(blue and purple) measuring between 8 and 24 centimeters (3 to 9 inches) lower than average in the eastern North Pacific, from the Gulf of Alaska to central Alaska, and along the equator. Unusual conditions persist in the western and mid-latitude Pacific Ocean as well, with higher than average sea-surface heights(red and white) of between 8 and 24 centimeters (3 to 9 inches). These areas of increased sea-surface height and unusually warm water were present last year, but the increase in height has surpassed last year's measurements. The TOPEX/Poseidon satellite's measurements over the last seven and a half years have provided scientists with a comprehensive record of the 1997-1999 El Niño/La Niña climate pattern by measuring changing sea-surface heights to within 4centimeters (1.5 inches) precision. The U.S./French mission is managed by the Jet Propulsion Laboratory for NASA's Earth Sciences Enterprise, Washington, DC. JPL is a division of the California Institute of Technology, Pasadena, CA. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov/ |
|
Pacific Decadal Oscillation
PIA03460
Sol (our sun)
Altimeter
| Title |
Pacific Decadal Oscillation |
| Original Caption Released with Image |
Like fall and winter of 2000, this year's Topex/Poseidon satellite data shows that the Pacific ocean continues to be dominated by the strong Pacific Decadal Oscillation, which is larger than the El Niño/La Niña pattern. The data, taken during a ten-day collection cycle ending Oct. 29,2001, show that the near-equatorial ocean has been very quiet in the past year, and sea levels and sea surface temperatures are near normal. Above-normal sea surface heights and warmer ocean temperatures, indicated by the red and white areas, still blanket the far western tropical Pacific and much of the north mid-Pacific. Red areas are about 10 centimeters (4inches) above normal, white areas show the sea surface height is between 14 and 32 centimeters (6 to 13 inches) above normal. In the western Pacific, the buildup of the Pacific Decadal Oscillation pattern, first noted by Topex/Poseidon oceanographers more than three years ago, has outlasted both the El Niño and La Niña of the past few years. This warmth contrasts with the Bering Sea, Gulf of Alaska and the west coast of the United States, where lower than normal sea surface levels and cool ocean temperatures continue, as indicated by the blue areas. The blue areas are between 5 and 13 centimeters (2 and 5 inches) below normal, while the purple areas range from 14 to 18 centimeters (6 to 7 inches) below normal. According to oceanographer Dr. William Patzert of NASA's Jet Propulsion Laboratory, Pasadena, Calif., the striking similarity between data taken in 2000 and the same time period in 2001 indicates that winter weather forecasts for this year will be similar to last year. The joint U.S.-French Topex/Poseidon mission is managed by the JPL for NASA's Earth Science Enterprise, NASA Headquarters, Washington, D.C. JPL is a division of the California Institute of Technology in Pasadena. For more information on Topex/Poseidon, see the Topex/Poseidon Web Site [ http://topex-www.jpl.nasa.gov ]. |
|
TOPEX/El Niño Watch - El Niñ
…
PIA00837
Sol (our sun)
Altimeter
| Title |
TOPEX/El Niño Watch - El Niño Warm Water Pool Returns to Near Normal State, Mar, 14, 1998 |
| Original Caption Released with Image |
This image of the Pacific Ocean was produced using sea surface height measurements taken by the U.S.-French TOPEX/Poseidon satellite. The image shows sea surface height relative to normal ocean conditions on Mar. 14, 1998 and sea surface height is an indicator of the heat content of the ocean. The image shows that the sea surface height along the central equatorial Pacific has returned to a near normal state. Oceanographers indicate this is a classic pattern, typical of a mature El Niño condition. Remnants of the El Niño warm water pool, shown in red and white, are situated to the north and south of the equator. These sea surface height measurements have provided scientists with a detailed view of how the 1997-98 El Niño's warm pool behaves because the TOPEX/Poseidon satellite measures the changing sea surface height with unprecedented precision. In this image, the white and red areas indicate unusual patterns of heat storage, in the white areas, the sea surface is between 14 and 32 centimeters (6 to 13 inches) above normal, in the red areas, it's about 10 centimeters (4 inches) above normal. The green areas indicate normal conditions, while purple (the western Pacific) means at least 18 centimeters (7 inches) below normal sea level. The El Niño phenomenon is thought to be triggered when the steady westward blowing trade winds weaken and even reverse direction. This change in the winds allows a large mass of warm water (the red and white area) that is normally located near Australia to move eastward along the equator until it reaches the coast of South America. The displacement of so much warm water affects evaporation, where rain clouds form and, consequently, alters the typical atmospheric jet stream patterns around the world. Using satellite imagery, buoy and ship data, and a forecasting model of the ocean-atmosphere system, the National Oceanic and Atmospheric Administration, (NOAA), has continued to issue an advisory indicating the so-called El Niño weather conditions that have impacted much of the United States and the world are expected to remain through the spring. For more information, please visit the TOPEX/Poseidon project web page at http://topex-www.jpl.nasa.gov |
|
Pacific Climate Calm
PIA08501
Sol (our sun)
Altimeter
| Title |
Pacific Climate Calm |
| Original Caption Released with Image |
In early 2006, a weak La Niña event kept the temperatures in the Pacific Ocean along the equator a little cooler than normal. Atlantic Ocean hurricane forecasters were keeping an eye on the Pacific because La Niña events and the large-scale atmospheric changes that often go along with them can have a long-distance effect on hurricane formation in the Atlantic Ocean. But by April 2006, the La Niña had all but faded. The latest remote-sensing data from the NASA/French Jason satellite show near-normal conditions across the equatorial Pacific Ocean. This image shows Jason observations of sea surface height collected over a 10-day period centered on May 24, 2006. The height of the water relates to the temperature of the water, an indicator of the changing amount of heat stored in the ocean. As the ocean warms, its level rises, as it cools, its level falls. Yellow and red areas indicate where the waters are relatively warmer and have expanded above normal sea level. Green areas, which dominate the image, indicate near-normal sea level. Blue and purple areas show where the waters are relatively colder, and the sea level is lower than normal. The Jason satellite carries a dual-frequency radar altimeter. This instrument beams microwave pulses downward toward the Earth at frequencies of 13.6 and 5.3 Gigahertz. To determine the ocean's height, the instrument precisely measures the time it takes for the microwave pulses to bounce off the surface and return to the spacecraft. This measure, multiplied by the speed of light, gives the range from the satellite to the ocean surface. The Jason mission is a collaboration between the United States and France, managed jointly by NASA's Jet Propulsion Laboratory and the Centre National d'Etudes Spatiales (CNES). NASA's research on Earth's oceans using Jason and other space-based capabilities is conducted as a part of its Science Mission Directorate, to better understand and protect our home planet. For more information, visit the Jason website [ http://sealevel.jpl.nasa.gov/science/jason1-quick-look/index.html ]. |
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