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Hot Shot
title Hot Shot
description The black dot in this picture of the Sun is Mercury. The planet made a rare pass in front of the Sun on May 7, 2003. The SOHO and TRACE spacecraft were watching with all instruments. The spacecraft websites are among many with Mercury transit galleries. *Image Credit*: NASA Goddard Space Flight Center
The Carina Nebula: Star Birt …
Title The Carina Nebula: Star Birth in the Extreme
General Information What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. In celebration of the 17th anniversary of the launch and deployment of NASA's Hubble Space Telescope, a team of astronomers is releasing one of the largest panoramic images ever taken with Hubble's cameras. READ: Junior version of this article Amazing Space Learn about this story in the Star Witness, a science newspaper available on our sister site, Amazing Space. [ http://amazing-space.stsci.edu/news/archive/2007/02/ ] It is a 50-light-year-wide view of the central region of the Carina Nebula where a maelstrom of star birth &#151, and death &#151, is taking place. This image is a mosaic of the Carina Nebula assembled from 48 frames taken with Hubble's Advanced Camera for Surveys. The Hubble images were taken in the light of neutral hydrogen during March and July 2005. Color information was added with data taken in December 2001 and March 2003 at the Cerro Tololo Inter-American Observatory in Chile. Red corresponds to sulfur, green to hydrogen, and blue to oxygen emission.
Scene Identification Compare …
Title Scene Identification Compared to Clouds (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the scene identification as measured by CERES during 29 orbits on June 20 and 21 of 2003. By comparing the incoming solar radiation with the outgoing reflected and thermal radiation, it is possible to identify the type of area being viewed, whether it be land, clouds, ocean, or ice. This scene identification is used together with the radiation flux measurements to build up a complete picture of the Earth's energy budget over time.
Completed 2005-06-21
Scene Identification Compare …
Title Scene Identification Compared to Clouds (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the scene identification as measured by CERES during 29 orbits on June 20 and 21 of 2003. By comparing the incoming solar radiation with the outgoing reflected and thermal radiation, it is possible to identify the type of area being viewed, whether it be land, clouds, ocean, or ice. This scene identification is used together with the radiation flux measurements to build up a complete picture of the Earth's energy budget over time.
Completed 2005-06-21
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk.
Completed 2004-02-18
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk.
Completed 2004-02-18
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk.
Completed 2004-02-18
Outgoing Shortwave Flux Comp …
Title Outgoing Shortwave Flux Compared to Clouds (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the reflected solar radiation measured by CERES during 29 orbits on June 20 and 21 of 2003 over infrared cloud images for the same period. Reflected solar radiation is shortwave radiation, and the most intense reflection comes from clouds.
Completed 2005-06-20
Outgoing Shortwave Flux Comp …
Title Outgoing Shortwave Flux Compared to Clouds (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the reflected solar radiation measured by CERES during 29 orbits on June 20 and 21 of 2003 over infrared cloud images for the same period. Reflected solar radiation is shortwave radiation, and the most intense reflection comes from clouds.
Completed 2005-06-20
Instantaneous Outgoing Longw …
Title Instantaneous Outgoing Longwave Flux (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the outgoing thermal radiation measured by CERES during 29 orbits on June 20 and 21 of 2003. Thermal radiation is longwave radiation and depends on the temperature of the earth, with the most intense radiation coming from the warmest regions and the least from cold clouds in the atmosphere. Although cold clouds and the cold Antarctic night regions can be seen in this data, the Earth radiates pretty uniformly in the longwave bands because the atmosphere distributes the heat of the sun to the whole planet.
Completed 2005-02-01
Instantaneous Outgoing Longw …
Title Instantaneous Outgoing Longwave Flux (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the outgoing thermal radiation measured by CERES during 29 orbits on June 20 and 21 of 2003. Thermal radiation is longwave radiation and depends on the temperature of the earth, with the most intense radiation coming from the warmest regions and the least from cold clouds in the atmosphere. Although cold clouds and the cold Antarctic night regions can be seen in this data, the Earth radiates pretty uniformly in the longwave bands because the atmosphere distributes the heat of the sun to the whole planet.
Completed 2005-02-01
Global Sea Surface Temperatu …
Title Global Sea Surface Temperature from June, 2002 to September, 2003 (WMS)
Abstract The temperature of the surface of the world's oceans provides a clear indication of the state of the Earth's climate and weather. The AMSR-E instrument on the Aqua satellite measures the temperature of the top 1 millimeter of the ocean every day, even through the clouds. In this visualization sequence covering the period from June, 2002, to September, 2003, the most obvious effects are the north-south movement of warm regions across the equator due to the seasonal movement of the sun and the seasonal advance and retreat of the sea ice near the North and South poles. It is also possible to see the Gulf Stream, the warm river of water that parallels the east coast of the United States before heading towards northern Europe, in this data. Around January 1, 2003, a cooler than normal region of the ocean appears just to the west of Peru as part of a La Nina and flows westward, driven by the trade winds. The waves that appear on the edges of this cooler area are called tropical instability waves and can also be seen in the equatorial Atlantic Ocean about the same time.
Completed 2004-02-12
Global Sea Surface Temperatu …
Title Global Sea Surface Temperature from June, 2002 to September, 2003 (WMS)
Abstract The temperature of the surface of the world's oceans provides a clear indication of the state of the Earth's climate and weather. The AMSR-E instrument on the Aqua satellite measures the temperature of the top 1 millimeter of the ocean every day, even through the clouds. In this visualization sequence covering the period from June, 2002, to September, 2003, the most obvious effects are the north-south movement of warm regions across the equator due to the seasonal movement of the sun and the seasonal advance and retreat of the sea ice near the North and South poles. It is also possible to see the Gulf Stream, the warm river of water that parallels the east coast of the United States before heading towards northern Europe, in this data. Around January 1, 2003, a cooler than normal region of the ocean appears just to the west of Peru as part of a La Nina and flows westward, driven by the trade winds. The waves that appear on the edges of this cooler area are called tropical instability waves and can also be seen in the equatorial Atlantic Ocean about the same time.
Completed 2004-02-12
GOES/SXI views the Sun in X- …
Title GOES/SXI views the Sun in X-rays (3 Channels)
Abstract The Solar X-ray Imager (SXI) aboard GOES-12 went online for full-time operation on January 22, 2003. It provides full-disk X-ray images of the Sun updated every few minutes. This movie combines three channels from the imager with red covering 0.6-2.0 nanometers wavelength, green covering 0.6-4.0 nanometers wavelength, and blue covering ~0.6-6.0 nanometers wavelength.
Completed 2003-01-29
GOES/SXI views the Sun in X- …
Title GOES/SXI views the Sun in X-rays (3 Channels)
Abstract The Solar X-ray Imager (SXI) aboard GOES-12 went online for full-time operation on January 22, 2003. It provides full-disk X-ray images of the Sun updated every few minutes. This movie combines three channels from the imager with red covering 0.6-2.0 nanometers wavelength, green covering 0.6-4.0 nanometers wavelength, and blue covering ~0.6-6.0 nanometers wavelength.
Completed 2003-01-29
Incoming Solar Flux Compared …
Title Incoming Solar Flux Compared to Clouds (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the incoming solar radiation within view of CERES during 29 orbits on June 20 and 21 of 2003. Because this is incoming solar flux, its magnitude only depends on the position of the sun, and, because the orbit is synchronized with the sun, the orbit crosses the equator in the daylight at about 1:30 PM local time on every orbit. This data is not actually measured from CERES, but is calculated to compare with the outgoing radiation that CERES does measure. Note that the infrared cloud image shown under the solar data shows high infrared as dark (land) and low infrared as light (clouds).
Completed 2005-06-21
Incoming Solar Flux Compared …
Title Incoming Solar Flux Compared to Clouds (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the incoming solar radiation within view of CERES during 29 orbits on June 20 and 21 of 2003. Because this is incoming solar flux, its magnitude only depends on the position of the sun, and, because the orbit is synchronized with the sun, the orbit crosses the equator in the daylight at about 1:30 PM local time on every orbit. This data is not actually measured from CERES, but is calculated to compare with the outgoing radiation that CERES does measure. Note that the infrared cloud image shown under the solar data shows high infrared as dark (land) and low infrared as light (clouds).
Completed 2005-06-21
Instantaneous Scene Identifi …
Title Instantaneous Scene Identification (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to th e climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the scene identification as measured by CERES during 29 orbits on June 20 and 21 of 2003. By comparing the incoming solar radiation with the outgoing reflected and thermal radiation, it is possible to identify the type of area being viewed, whether it be land, clouds, ocean, or ice. This scene identification is used together with the radiation flux measurements to build up a complete picture of the Earth's energy budget over time.
Completed 2005-02-01
Instantaneous Scene Identifi …
Title Instantaneous Scene Identification (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to th e climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the scene identification as measured by CERES during 29 orbits on June 20 and 21 of 2003. By comparing the incoming solar radiation with the outgoing reflected and thermal radiation, it is possible to identify the type of area being viewed, whether it be land, clouds, ocean, or ice. This scene identification is used together with the radiation flux measurements to build up a complete picture of the Earth's energy budget over time.
Completed 2005-02-01
Instantaneous Incoming Solar …
Title Instantaneous Incoming Solar Flux (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the incoming solar radiation within view of CERES during 29 orbits on June 20 and 21 of 2003. Because this is incoming solar flux, its magnitude only depends on the position of the sun, and, because the orbit is synchronized with the sun, the orbit crosses the equator in the daylight at about 1:30 PM local time on every orbit. This data is not actually measured from CERES, but is calculated to compare with the outgoing radiation that CERES does measure.
Completed 2005-02-01
Instantaneous Incoming Solar …
Title Instantaneous Incoming Solar Flux (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth rotates, the sun lights up only part of the Earth at a time, and some of that incoming solar energy is reflected and some is absorbed, depending on type of area it lights. The amount of reflection and absorption is critical to the climate. An instrument named CERES orbits the Earth every 99 minutes and measures the reflected solar energy. This animation shows the incoming solar radiation within view of CERES during 29 orbits on June 20 and 21 of 2003. Because this is incoming solar flux, its magnitude only depends on the position of the sun, and, because the orbit is synchronized with the sun, the orbit crosses the equator in the daylight at about 1:30 PM local time on every orbit. This data is not actually measured from CERES, but is calculated to compare with the outgoing radiation that CERES does measure.
Completed 2005-02-01
NASA's Orbiting Earth Observ …
Title NASA's Orbiting Earth Observing Fleet
Abstract While NASA is actively exploring Mars with new landers and orbiters, it's exciting to consider that it already maintains a powerful and diverse fleet around the Earth. NASA's Earth Observing fleet of vehicles constitutes a major milestone in the history of Earth science, facilitating the kinds of wide scale and synergistic research endeavors that until the last decade have been impossible to even consider. Many of the techniques being employed around Earth are a direct offshoot of technological and scientific techniques developed on missions to other worlds. As the Red planet looms large in our view screens, we reflect that NASA's continued commitment to primary research about our home remains a top priority not only to the agency, but to the nation, and the world as a whole. This visualization shows the spacecraft in NASA's Earth Observing fleet. The relative altitudes, speeds, and sun position are correct for 12-01-2003 starting at 5:00 UTC.
Completed 2003-12-18
NASA's Orbiting Earth Observ …
Title NASA's Orbiting Earth Observing Fleet
Abstract While NASA is actively exploring Mars with new landers and orbiters, it's exciting to consider that it already maintains a powerful and diverse fleet around the Earth. NASA's Earth Observing fleet of vehicles constitutes a major milestone in the history of Earth science, facilitating the kinds of wide scale and synergistic research endeavors that until the last decade have been impossible to even consider. Many of the techniques being employed around Earth are a direct offshoot of technological and scientific techniques developed on missions to other worlds. As the Red planet looms large in our view screens, we reflect that NASA's continued commitment to primary research about our home remains a top priority not only to the agency, but to the nation, and the world as a whole. This visualization shows the spacecraft in NASA's Earth Observing fleet. The relative altitudes, speeds, and sun position are correct for 12-01-2003 starting at 5:00 UTC.
Completed 2003-12-18
Closeup of Solar 'Tadpoles' …
Title Closeup of Solar 'Tadpoles' with time tags
Abstract Here is a close-up view of dark 'tentacles' or 'tadpoles' moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE. One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare. This version of the visualization displays the instrument clock time tags.
Completed 2003-03-26
Closeup of Solar 'Tadpoles' …
Title Closeup of Solar 'Tadpoles' with time tags
Abstract Here is a close-up view of dark 'tentacles' or 'tadpoles' moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE. One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare. This version of the visualization displays the instrument clock time tags.
Completed 2003-03-26
Closeup of Solar 'Tadpoles' …
Title Closeup of Solar 'Tadpoles' with time tags
Abstract Here is a close-up view of dark 'tentacles' or 'tadpoles' moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE. One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare. This version of the visualization displays the instrument clock time tags.
Completed 2003-03-26
Closeup of Solar 'Tadpoles' …
Title Closeup of Solar 'Tadpoles' with time tags
Abstract Here is a close-up view of dark 'tentacles' or 'tadpoles' moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE. One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare. This version of the visualization displays the instrument clock time tags.
Completed 2003-03-26
Connections: Terrestrial Gam …
Title Connections: Terrestrial Gamma Flashes and Lightning?
Abstract The RHESSI instrument not only views the Sun but can detect gamma-rays from sources on Earth as well.
Completed 2005-02-10
Halloween Solar Storms from …
Title Halloween Solar Storms from SOHO/EIT, 195 Angstroms
Abstract This view from SOHO/EIT in the 195 Angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002960) and 2961 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002961). For more information on how X-ray solar flares are classified (B, C, M, X), visit (http://www.spaceweather.com/glossary/flareclasses.html).
Completed 2004-07-08
Halloween Solar Storms from …
Title Halloween Solar Storms from SOHO/EIT, 195 Angstroms
Abstract This view from SOHO/EIT in the 195 Angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002960) and 2961 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002961). For more information on how X-ray solar flares are classified (B, C, M, X), visit (http://www.spaceweather.com/glossary/flareclasses.html).
Completed 2004-07-08
Halloween Solar Storms from …
Title Halloween Solar Storms from SOHO/EIT, 195 Angstroms
Abstract This view from SOHO/EIT in the 195 Angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002960) and 2961 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002961). For more information on how X-ray solar flares are classified (B, C, M, X), visit (http://www.spaceweather.com/glossary/flareclasses.html).
Completed 2004-07-08
Halloween Solar Storms from …
Title Halloween Solar Storms from SOHO/EIT, 195 Angstroms
Abstract This view from SOHO/EIT in the 195 Angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002960) and 2961 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002961). For more information on how X-ray solar flares are classified (B, C, M, X), visit (http://www.spaceweather.com/glossary/flareclasses.html).
Completed 2004-07-08
Halloween Solar Storms from …
Title Halloween Solar Storms from SOHO/EIT, 195 Angstroms
Abstract This view from SOHO/EIT in the 195 Angstrom band, shows the multitude of solar flares released in the Fall of 2003 as a group of active regions rotated back into view. This movie is synchronized to play with animation IDs 2960 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002960) and 2961 (http://svs.gsfc.nasa.gov/vis/a000000/a002900/a002961). For more information on how X-ray solar flares are classified (B, C, M, X), visit (http://www.spaceweather.com/glossary/flareclasses.html).
Completed 2004-07-08
The Visible Sun Revisited
Title The Visible Sun Revisited
Abstract Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar farside (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions "before" they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts.
Completed 2006-02-07
The Visible Sun Revisited
Title The Visible Sun Revisited
Abstract Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar farside (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions "before" they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts.
Completed 2006-02-07
The Visible Sun Revisited
Title The Visible Sun Revisited
Abstract Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar farside (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions "before" they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts.
Completed 2006-02-07
The Visible Sun Revisited
Title The Visible Sun Revisited
Abstract Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar farside (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions "before" they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts.
Completed 2006-02-07
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares - Video version
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. This version has the contents slightly smaller for use in video.
Completed 2004-02-18
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares - Video version
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. This version has the contents slightly smaller for use in video.
Completed 2004-02-18
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares - Video version
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. This version has the contents slightly smaller for use in video.
Completed 2004-02-18
SORCE Monitors Solar Variabi …
Title SORCE Monitors Solar Variability during Record Solar Flares - Video version
Abstract The SORCE mission monitors solar variability to determine its impact on the Earth's climate. The X-ray photometer aboard SORCE observes the record-breaking solar flares in the Fall of 2003. The line graph shows the photometer's measured solar radiation flux in the 1-7 nanometer wavelength band (x-ray) measured in milliwatts per square meter. The ultraviolet (195 Angstrom) imagery from SOHO/EIT (green) illustrates where the flares (the bright white spots) are located on the solar disk. This version has the contents slightly smaller for use in video.
Completed 2004-02-18
NASA's Orbiting Earth Observ …
Title NASA's Orbiting Earth Observing Fleet (improved background)
Abstract NASA's Earth Observing fleet of vehicles constitutes a major milestone in the history of Earth science, facilitating the kinds of wide scale and synergistic research endeavors that until the last decade have been impossible to even consider. Many of the techniques being employed around Earth are a direct offshoot of technological and scientific techniques developed on missions to other worlds. NASA's continued commitment to primary research about our home remains a top priority not only to the agency, but to the nation, and the world as a whole. This visualization shows the spacecraft in NASA's Earth Observing fleet. The relative altitudes, speeds, and sun position are correct for 12-01-2003 starting at 5:00 UTC. Aura was added as it would have appeared in orbit had it already been launched at that time. This is an HD version that uses an earth with clouds.
Completed 2005-09-02
The fastest CME of Cycle 23 …
Title The fastest CME of Cycle 23 overtakes another fast CME
Abstract On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft.
Completed 2004-05-13
The fastest CME of Cycle 23 …
Title The fastest CME of Cycle 23 overtakes another fast CME
Abstract On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft.
Completed 2004-05-13
The fastest CME of Cycle 23 …
Title The fastest CME of Cycle 23 overtakes another fast CME
Abstract On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft.
Completed 2004-05-13
The fastest CME of Cycle 23 …
Title The fastest CME of Cycle 23 overtakes another fast CME
Abstract On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft.
Completed 2004-05-13
The fastest CME of Cycle 23 …
Title The fastest CME of Cycle 23 overtakes another fast CME
Abstract On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft.
Completed 2004-05-13
Solar Irradiance (WMS)
Title Solar Irradiance (WMS)
Abstract The Earth's climate is determined by energy transfer from the sun to the Earth's land, oceans, and atmosphere. As the Earth moves around the sun, the fact that the Earth's axis is tilted means that the sun's overhead position moves from the Northern Hemisphere to the Southern Hemisphere and back from one summer to the next. This effect causes winters to be cold and summers warm in the Northern Hemisphere and the opposite in the Southern Hemisphere. This animation shows the incoming solar irradiance on the Earth at noon on the Greenwich meridian during an entire year, illustrating this movement. The magnitude of this irradiance comes from measurements by the TIM instrument on SORCE. Since the Earth's orbit is elliptical, the magnitude of the solar irradiance at the Earth is least when the Earth is farthest from the sun and greatest when the earth is closest. This 6 or 7 percent change can be seen in the animation by watching the dark bands move. When the bands expand from the bright spot, the Earth is getting closer to the sun, from July through December, and when they contract the Earth is moving away, from January through June. The sun's irradiance is also variable from day to day, but that effect is about ten times smaller than the effect of the earth's orbit.
Completed 2005-02-28
NASA's Orbiting Earth Observ …
Title NASA's Orbiting Earth Observing Fleet (includes Aura)
Abstract NASA's Earth Observing fleet of vehicles constitutes a major milestone in the history of Earth science, facilitating the kinds of wide scale and synergistic research endeavors that until the last decade have been impossible to even consider. Many of the techniques being employed around Earth are a direct offshoot of technological and scientific techniques developed on missions to other worlds. NASA's continued commitment to primary research about our home remains a top priority not only to the agency, but to the nation, and the world as a whole. This visualization shows the spacecraft in NASA's Earth Observing fleet. The relative altitudes, speeds, and sun position are correct for 12-01-2003 starting at 5:00 UTC. Aura was added as it would appear in orbit (if it were in orbit at this time).
Completed 2004-05-13
NASA's Orbiting Earth Observ …
Title NASA's Orbiting Earth Observing Fleet (includes Aura)
Abstract NASA's Earth Observing fleet of vehicles constitutes a major milestone in the history of Earth science, facilitating the kinds of wide scale and synergistic research endeavors that until the last decade have been impossible to even consider. Many of the techniques being employed around Earth are a direct offshoot of technological and scientific techniques developed on missions to other worlds. NASA's continued commitment to primary research about our home remains a top priority not only to the agency, but to the nation, and the world as a whole. This visualization shows the spacecraft in NASA's Earth Observing fleet. The relative altitudes, speeds, and sun position are correct for 12-01-2003 starting at 5:00 UTC. Aura was added as it would appear in orbit (if it were in orbit at this time).
Completed 2004-05-13
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