|
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IBEX Heliosphere Map - 2.8 t
…
The Interstellar Boundary Ex
…
10/15/09
| Description |
The Interstellar Boundary Explorer (IBEX) mission is a NASA-funded satellite that orbits Earth and maps the boundary of our Solar System from Earth's point of view looking outward. IBEX has completed the first all-sky maps of this boundary by detecting particles traveling inward from the boundary toward our region of the Solar System. The map appears to be oval in shape for the same reason that two-dimensional maps of spherical Earth look oval. The boundary of our Solar System is created by the interaction between charged particles from the Sun that are streaming outward, called the solar wind, and material between the stars, called the interstellar medium (ISM). The solar wind flows outward into space and carves out a protective bubble, called the heliosphere, in the ISM around our Solar System. At the boundary, the interactions between the solar wind particles and the ISM particles create energetic neutral atoms (ENAs). ENAs are particles with no charge that move very fast. Some of the ENAs happen to be traveling in just the right way so that they move inward through the Solar System toward Earth where IBEX can collect them. Using two sensors, called IBEX-Hi and IBEX-Lo, the spacecraft measures and counts these ENAs. The scientists can create maps of the boundary using this information. For each small area of the sky, IBEX has measured the number of ENAs coming from that direction. This map shows the distribution of ENAs ranging in energy from 2.8 to 5.6 keV. Red indicates the highest number of ENAs measured by the spacecraft. Yellow and green indicate lower numbers of ENAs, and blue and purple show the lowest number of ENAs. |
| Date |
10/15/09 |
|
IBEX Heliosphere Map - 0.6 t
…
The Interstellar Boundary Ex
…
10/15/09
| Description |
The Interstellar Boundary Explorer (IBEX) mission is a NASA-funded satellite that orbits Earth and maps the boundary of our Solar System from Earth's point of view looking outward. IBEX has completed the first all-sky maps of this boundary by detecting particles traveling inward from the boundary toward our region of the Solar System. The map appears to be oval in shape for the same reason that two-dimensional maps of spherical Earth look oval. The boundary of our Solar System is created by the interaction between charged particles from the Sun that are streaming outward, called the solar wind, and material between the stars, called the interstellar medium (ISM). The solar wind flows outward into space and carves out a protective bubble, called the heliosphere, in the ISM around our Solar System. At the boundary, the interactions between the solar wind particles and the ISM particles create energetic neutral atoms (ENAs). ENAs are particles with no charge that move very fast. Some of the ENAs happen to be traveling in just the right way so that they move inward through the Solar System toward Earth where IBEX can collect them. Using two sensors, called IBEX-Hi and IBEX-Lo, the spacecraft measures and counts these ENAs. The scientists can create maps of the boundary using this information. For each small area of the sky, IBEX has measured the number of ENAs coming from that direction. This map shows the distribution of ENAs ranging in energy from 0.6 to 1.0 keV. Red indicates the highest number of ENAs measured by the spacecraft. Yellow and green indicate lower numbers of ENAs, and blue and purple show the lowest number of ENAs. |
| Date |
10/15/09 |
|
IBEX Heliosphere Map - 1.3 t
…
The Interstellar Boundary Ex
…
10/15/09
| Description |
The Interstellar Boundary Explorer (IBEX) mission is a NASA-funded satellite that orbits Earth and maps the boundary of our Solar System from Earth's point of view looking outward. IBEX has completed the first all-sky maps of this boundary by detecting particles traveling inward from the boundary toward our region of the Solar System. The map appears to be oval in shape for the same reason that two-dimensional maps of spherical Earth look oval. The boundary of our Solar System is created by the interaction between charged particles from the Sun that are streaming outward, called the solar wind, and material between the stars, called the interstellar medium (ISM). The solar wind flows outward into space and carves out a protective bubble, called the heliosphere, in the ISM around our Solar System. At the boundary, the interactions between the solar wind particles and the ISM particles create energetic neutral atoms (ENAs). ENAs are particles with no charge that move very fast. Some of the ENAs happen to be traveling in just the right way so that they move inward through the Solar System toward Earth where IBEX can collect them. Using two sensors, called IBEX-Hi and IBEX-Lo, the spacecraft measures and counts these ENAs. The scientists can create maps of the boundary using this information. For each small area of the sky, IBEX has measured the number of ENAs coming from that direction. This map shows the distribution of ENAs ranging in energy from 1.3 to 2.4 keV. Red indicates the highest number of ENAs measured by the spacecraft. Yellow and green indicate lower numbers of ENAs, and blue and purple show the lowest number of ENAs. |
| Date |
10/15/09 |
|
IBEX Heliosphere Map - 1.9 t
…
The Interstellar Boundary Ex
…
10/15/09
| Description |
The Interstellar Boundary Explorer (IBEX) mission is a NASA-funded satellite that orbits Earth and maps the boundary of our Solar System from Earth's point of view looking outward. IBEX has completed the first all-sky maps of this boundary by detecting particles traveling inward from the boundary toward our region of the Solar System. The map appears to be oval in shape for the same reason that two-dimensional maps of spherical Earth look oval. The boundary of our Solar System is created by the interaction between charged particles from the Sun that are streaming outward, called the solar wind, and material between the stars, called the interstellar medium (ISM). The solar wind flows outward into space and carves out a protective bubble, called the heliosphere, in the ISM around our Solar System. At the boundary, the interactions between the solar wind particles and the ISM particles create energetic neutral atoms (ENAs). ENAs are particles with no charge that move very fast. Some of the ENAs happen to be traveling in just the right way so that they move inward through the Solar System toward Earth where IBEX can collect them. Using two sensors, called IBEX-Hi and IBEX-Lo, the spacecraft measures and counts these ENAs. The scientists can create maps of the boundary using this information. For each small area of the sky, IBEX has measured the number of ENAs coming from that direction. This map shows the distribution of ENAs ranging in energy from 1.9 to 3.6 keV. Red indicates the highest number of ENAs measured by the spacecraft. Yellow and green indicate lower numbers of ENAs, and blue and purple show the lowest number of ENAs. |
| Date |
10/15/09 |
|
IBEX Heliosphere Map - 0.9 t
…
The Interstellar Boundary Ex
…
10/15/09
| Description |
The Interstellar Boundary Explorer (IBEX) mission is a NASA-funded satellite that orbits Earth and maps the boundary of our Solar System from Earth's point of view looking outward. IBEX has completed the first all-sky maps of this boundary by detecting particles traveling inward from the boundary toward our region of the Solar System. The map appears to be oval in shape for the same reason that two-dimensional maps of spherical Earth look oval. The boundary of our Solar System is created by the interaction between charged particles from the Sun that are streaming outward, called the solar wind, and material between the stars, called the interstellar medium (ISM). The solar wind flows outward into space and carves out a protective bubble, called the heliosphere, in the ISM around our Solar System. At the boundary, the interactions between the solar wind particles and the ISM particles create energetic neutral atoms (ENAs). ENAs are particles with no charge that move very fast. Some of the ENAs happen to be traveling in just the right way so that they move inward through the Solar System toward Earth where IBEX can collect them. Using two sensors, called IBEX-Hi and IBEX-Lo, the spacecraft measures and counts these ENAs. The scientists can create maps of the boundary using this information. For each small area of the sky, IBEX has measured the number of ENAs coming from that direction. This map shows the distribution of ENAs ranging in energy from 0.9 to 1.5 keV. Red indicates the highest number of ENAs measured by the spacecraft. Yellow and green indicate lower numbers of ENAs, and blue and purple show the lowest number of ENAs. |
| Date |
10/15/09 |
|
Multi-angle Images of Hudson
…
At left is a true-color imag
…
| Description |
At left is a true-color image from the downward-looking (nadir) camera on the Multi-angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. The false-color image at right is a composite of red band data taken by the MISR forward 45.6-degree, nadir, and aftward 45.6-degree cameras, displayed in blue, green, and red colors, respectively. Color variations in the left image highlight spectral (true-color) differences, whereas those in the right image highlight differences in angular reflectance properties. The purple areas in the right image are low cloud, and light blue at the edge of the bay is due to increased forward scattering by the fast (smooth) ice. The orange areas are rougher ice, which scatters more light in the backward direction. This example illustrates how multi-angle viewing can distinguish physical structures and textures. Data for all channels are presented in a Space Oblique Mercator map projection to facilitate their co- registration. The images are about 400 km (250 miles) wide with a spatial resolution of about 275 meters (300 yards). North is toward the top. MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Office of Earth Science, Washington, DC. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, MD. JPL is a division of the California Institute of Technology. ##### |
|
Exotic World Blisters Under
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| Title |
Exotic World Blisters Under the Sun |
| Description |
This artist's concept shows a Jupiter-like planet soaking up the scorching rays of its nearby "sun." NASA's Spitzer Space Telescope used its heat-seeking infrared eyes to figure out that a gas-giant planet like the one depicted here is two-faced, with one side perpetually in the cold dark, and the other forever blistering under the heat of its star. The illustration portrays how the planet would appear to infrared eyes, showing temperature variations across its surface. The planet, called Upsilon Andromedae b, was first discovered in 1996 around the star Upsilon Andromedae, located 40 light-years away in the constellation Andromeda. This star also has two other planets orbiting farther out. Upsilon Andromedae b is what's known as a "hot-Jupiter" planet, because it is made of gas like our Jovian giant, and it is hot, due to its tight, 4.6-day-long jaunt around its star. The toasty planet orbits at one-sixth the distance of Mercury from our own sun. It travels in a plane that is seen neither edge- nor face-on from our solar system, but somewhere in between. Scientists do not know how fast Upsilon Andromedae b is spinning on its axis, but they believe that it is tidally locked to its star, just as our locked moon forever hides its "dark side" from Earth's view. Spitzer observed Upsilon Andromedae b at five points during the planet's trip around its star. The planet's light levels went up or down, as detected by Spitzer, depending on whether the planet's sunlit or dark side was pointed toward Earth. These data indicate that the temperature difference between the two hemispheres of the planet is about 1,400 degrees Celsius (2,550 degrees Fahrenheit). According to astronomers, this means that the side of the planet that faces the star is always as hot as lava, while the other side could potentially be as cold as ice. Specifically, the hot side of the planet ranges from about 1,400 to 1,650 degrees Celsius (2,550 to 3,000 degrees Fahrenheit), and the cold side from about minus 20 to 230 degrees Celsius (minus 4 to 450 degrees Fahrenheit). How can one side always be hot? The atmosphere of the planet must be absorbing and reradiating light fast enough that any heated gas circulating around the planet is cooled off before it reaches the dark side. |
|
Saturn's Magnetosphere
| Description |
Saturn's Magnetosphere |
| Full Description |
The magnetosphere is an area of space, around a planet, that is controlled by that planet's magnetic field. Saturn is surrounded by a giant magnetic field, lined up with the rotation axis of the planet. This cannot be explained by current theories. Cassini may explain how the puzzling magnetic field of Saturn is generated. This magnetic field may also cause strange features in the rings called 'spokes'. These markings fall across the rings like spokes in a wheel and may be caused by electrically charged particles caught up in the magnetic field, but there are as yet no detailed theories about them. The brief reconnaissance encounters of the Pioneer 11 and the two Voyager spacecraft have provided most of our current information about the structure and dynamics of Saturn's magnetosphere. Here are some things that we do know: * Saturn's 'bow shock', the region point where the solar wind and the planet's magnetic field meet, much like the bow wave of a ship, is between 20 and 35 times Saturn's radius out into space. * The thickness of the bow shock is about 2000 kilometres. * Saturn's internal magnetic field is closely aligned with the planet's axis of rotation (within 1 degree). Saturn's magnetosphere appears to be intermediate in nature to those of Earth and Jupiter. As with Jupiter's magnetosphere, the dayside inner magnetosphere is mostly driven by the fast planetary rotation. However at night, it is expected that the nightside and outer magnetosphere is primarily driven by the solar wind, as is the case on Earth. * There is an electrical current (the 'equatorial ring current') flowing with about 10 000 000 Amps around 600 000 kilometres above Saturn. * Saturn Kilometric Radiation (SKR) is the principal radio emission from Saturn. SKR is believed to be linked to the way electrons in the solar wind interact with the magnetic field at Saturn's poles. Click here for a high resolution version. *Credit:* ESA |
| Date |
June 2, 2004 |
|
Saturn's Magnetosphere
| Description |
Saturn's Magnetosphere |
| Full Description |
The magnetosphere is an area of space, around a planet, that is controlled by that planet's magnetic field. Saturn is surrounded by a giant magnetic field, lined up with the rotation axis of the planet. This cannot be explained by current theories. Cassini may explain how the puzzling magnetic field of Saturn is generated. This magnetic field may also cause strange features in the rings called 'spokes'. These markings fall across the rings like spokes in a wheel and may be caused by electrically charged particles caught up in the magnetic field, but there are as yet no detailed theories about them. The brief reconnaissance encounters of the Pioneer 11 and the two Voyager spacecraft have provided most of our current information about the structure and dynamics of Saturn's magnetosphere. Here are some things that we do know: * Saturn's 'bow shock', the region point where the solar wind and the planet's magnetic field meet, much like the bow wave of a ship, is between 20 and 35 times Saturn's radius out into space. * The thickness of the bow shock is about 2000 kilometres. * Saturn's internal magnetic field is closely aligned with the planet's axis of rotation (within 1 degree). Saturn's magnetosphere appears to be intermediate in nature to those of Earth and Jupiter. As with Jupiter's magnetosphere, the dayside inner magnetosphere is mostly driven by the fast planetary rotation. However at night, it is expected that the nightside and outer magnetosphere is primarily driven by the solar wind, as is the case on Earth. * There is an electrical current (the 'equatorial ring current') flowing with about 10 000 000 Amps around 600 000 kilometres above Saturn. * Saturn Kilometric Radiation (SKR) is the principal radio emission from Saturn. SKR is believed to be linked to the way electrons in the solar wind interact with the magnetic field at Saturn's poles. Click here for a high resolution version. *Credit:* ESA |
| Date |
June 2, 2004 |
|
| Description |
Here on the Gallery page you can find the very latest images, videos and products from the Cassini-Huygens mission to Saturn, including the spectacular launch, spacecraft assembly and the exciting trip to Saturn. |
| Full Description |
This sequence of nine true-color, narrow-angle images shows the varying appearance of Jupiter as it rotated through more than a complete 360-degree turn. The smallest features seen in this sequence are no bigger than about 380 kilometers (about 236 miles). Rotating more than twice as fast as Earth, Jupiter completes one rotation in about 10 hours. These images were taken on Oct. 22 and 23, 2000. From image to image (proceeding left to right across each row and then down to the next row), cloud features on Jupiter move from left to right before disappearing over the edge onto the nightside of the planet. The most obvious Jovian feature is the Great Red Spot, which can be seen moving onto the dayside in the third frame (below and to the left of the center of the planet). In the fourth frame, taken about 1 hour and 40 minutes later, the Great Red Spot has been carried by the planet's rotation to the east and does not appear again until the final frame, which was taken one complete rotation after the third frame. Unlike weather systems on Earth, which change markedly from day to day, large cloud systems in Jupiter's colder, thicker atmosphere are long-lived, so the two frames taken one rotation apart have a very similar appearance. However, when this sequence of images is eventually animated, strong winds blowing eastward at some latitudes and westward at other latitudes will be readily apparent. The results of such differential motions can be seen even in the still frames shown here. For example, the clouds of the Great Red Spot rotate counterclockwise. The strong westward winds northeast of the Great Red Spot are deflected around the spot and form a wake of turbulent clouds downstream (visible in the fourth image), just as a rock in a rapidly flowing river deflects the fluid around it. The equatorial zone on Jupiter is currently bright white, indicating the presence of clouds much like cirrus clouds on Earth, but made of ammonia instead of water ice. This is very different from Jupiter's appearance 20 years ago, when the equatorial zone was more of a brownish cast similar to the region just to its north. At the northern edge of the equatorial zone, local regions colored a dark grayish-blue are places where the ammonia clouds have cleared allowing a view to deeper levels in Jupiter's atmosphere. Interrupting these relatively clear regions is a series of bright arrow-shaped equatorial plumes. The most obvious one is visible just above and to the right of center in the third and ninth frames. These plumes resemble the `anvil' clouds that accompany common summer thunderstorms on Earth, although the Jovian plumes are much bigger, and their somewhat regular spacing around the planet suggests an association with a planetary-scale wave motion. The southwest-northeast tilt of these plumes suggests that the winds in this region act to help maintain the eastward winds at this latitude. In the dark belt north of the equatorial zone, a turbulent, region with a white filamentary cloud is visible in the sixth frame, indicating rapidly changing wind direction. Several white ovals are visible at higher southern latitudes (toward the bottom of the fourth, fifth, and sixth frames, for example). These ovals, like the Great Red Spot, rotate counterclockwise and are similar in some respects to high-pressure systems on Earth. When these images were taken, Cassini was about 3.3 degrees above Jupiter's equatorial plane, and the Sun-Jupiter-spacecraft angle was about 20 degrees. JPL manages the Cassini mission for NASA's Office of Space Science, Washington, D.C. JPl is a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/University of Arizona. (PIA02825A) For higher resolution, click here. |
|
A Privileged View
| Description |
A Privileged View |
| Full Description |
From Saturn orbit, the Cassini spacecraft provides a perspective on the ringed planet that is never seen from Earth. In our skies, Saturn's disk is always nearly fully illuminated by the sun. From this vantage point -- nearly in the ringplane, with the sun over to the right -- the Cassini spacecraft can see both lit and dark hemispheres, with the shadow of the rings on the northern hemisphere. Saturn's low density and fast rotation cause its shape to deviate from spherical to a pronounced oblateness, very apparent here. The image was taken using the Cassini spacecraft wide-angle camera and a filter sensitive to wavelengths of infrared light centered at 728 nanometers. The image was acquired on Sept. 30, 2005, at a distance of approximately 2.4 million kilometers (1.5 million miles) from Saturn and at a Sun-Saturn-spacecraft, or phase, angle of 79 degrees. The mage scale is 139 kilometers (86 miles) per pixel. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . *Credit: *NASA/JPL/Space Science Institute |
| Date |
November 11, 2005 |
|
Aurora Australis
| title |
Aurora Australis |
| description |
Red and green colors predominate in this view of the Aurora Australis photographed from the Space Shuttle in May 1991 at the peak of the last geomagnetic maximum. The payload bay and tail of the Shuttle can be seen on the left hand side of the picture. Auroras are caused when high-energy electrons pour down from the Earth's magnetosphere and collide with atoms. Red aurora occurs from 200 km to as high as 500 km altitude and is caused by the emission of 6300 Angstrom wavelength light from oxygen atoms. Green aurora occurs from about 100 km to 250 km altitude and is caused by the emission of 5577 Angstrom wavelength light from oxygen atoms. The light is emitted when the atoms return to their original unexcited state. At times of peaks in solar activity, there are more geomagnetic storms and this increases the auroral activity viewed on Earth and by astronauts from orbit. Photographing them requires careful technique with long exposures and fast film (in this case ASA 1600). Such film can only be used on short-duration Shuttle flights and not from the Space Station because it is sensitive to radiation damage in orbit over time. The most recent astronaut photograph of aurora was taken before the April 2001 flurry of solar activity, and showed only a relatively low-energy green glow. This image was taken by the crew of the Space Shuttle Discovery in May 1991. *Image Credit*: NASA |
|
Butterfly Nebula
| Title |
Butterfly Nebula |
| Full Description |
The Hubble Space Telescope's Wide Field and Planetary Camera 2 (WFPC2) is back at work, capturing this image of the "butterfly wing"- shaped nebula, NGC 2346. The nebula is about 2,000 light-years away from Earth in the direction of the constellation Monoceros. It represents the spectacular "last gasp" of a binary star system at the nebula's center. The image was taken on March 6, 1997 as part of the recommissioning of the Hubble Space Telescope's previously installed scientific instruments following the successful servicing of the HST by NASA shuttle astronauts in February. WFPC2 was installed in HST during the servicing mission in 1993. At the center of the nebula lies a pair of stars that are so close together that they orbit around each other every 16 days. This is so close that, even with Hubble, the pair of stars cannot be resolved into its two components. One component of this binary is the hot core of a star that has ejected most of its outer layers, producing the surrounding nebula. Astronomers believe that this star, when it evolved and expanded to become a red giant, actually swallowed its companion star in an act of stellar cannibalism. The resulting interaction led to a spiraling together of the two stars, culminating in ejection of the outer layers of the red giant. Most of the outer layers were ejected into a dense disk, which can still be seen in the Hubble image, surrounding the central star. Later the hot star developed a fast stellar wind. This wind, blowing out into the surrounding disk, has inflated the large, wispy hourglass-shaped wings perpendicular to the disk. These wings produce the butterfly appearance when seen in projection. The total diameter of the nebula is about one-third of a light-year, or 2 trillion miles. |
| Date |
03/06/1997 |
| NASA Center |
Hubble Space Telescope Center |
|
Hubble Reopens Eye on the Un
…
| Title |
Hubble Reopens Eye on the Universe |
| Full Description |
In its first glimpse of the heavens following the successful December 1999 servicing mission, NASA's Hubble Space Telescope captured a majestic view of a planetary nebula, the glowing remains of a dying, Sun-like star. This stellar relic, first spied by William Herschel in 1787, is nicknamed the "Eskimo" Nebula (NGC 2392) because, when viewed through ground-based telescopes, it resembles a face surrounded by a fur parka. In this Hubble telescope image, the "parka" is really a disk of material embellished with a ring of comet-shaped objects, with their tails streaming away from the central, dying star. The Eskimo's "face" also contains some fascinating details. Although this bright central region resembles a ball of twine, it is, in reality, a bubble of material being blown into space by the central star's intense "wind" of high-speed material. In this photo, one bubble lies in front of the other, obscuring part of the second lobe. Scientists believe that a ring of dense material around the star's equator, ejected during its red giant phase, created the nebula's shape. The bubbles are not smooth like balloons but have filaments of denser matter. Each bubble is about 1 light-year long and about half a light-year wide. Scientists are still puzzled about the origin of the comet-shaped features in the "parka." One possible explanation is that these objects formed from a collision of slow-and fast-moving gases. The Eskimo Nebula is about 5,000 light-years from Earth in the constellation Gemini. The picture was taken Jan. 10 and 11, 2000, with the Wide Field and Planetary Camera 2. The nebula's glowing gases produce the colors in this image: nitrogen (red), hydrogen (green), oxygen (blue), and helium (violet). |
| Date |
01/24/2000 |
| NASA Center |
Hubble Space Telescope Center |
|
Hubble Follows Rapid Changes
…
| Title |
Hubble Follows Rapid Changes in Jupiter's Aurora |
|
Hubble Camera Resumes Scienc
…
| Title |
Hubble Camera Resumes Science Operation with Picture of "Butterfly" in Space |
| General Information |
What is an Early Release Observation? A photograph of a celestial object that demonstrates the performance of a new Hubble camera. The Hubble telescope is back at work, capturing this view of the butterfly-wing-shaped nebula, NGC 2346. The nebula is about 2,000 light-years away from Earth in the direction of the constellation Monoceros. It represents the spectacular "last gasp" of a double-star system at the nebula's center. The image was taken March 6, 1997 as part of the re-commissioning of Hubble's previously installed scientific instruments following a successful servicing mission. |
|
Hubble Reveals Invisible Hig
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| Title |
Hubble Reveals Invisible High-Speed Collision around Supernova 1987A |
| General Information |
What is an American Astronomical Society Meeting release? A major news announcement issued at an American Astronomical Society meeting, the premier astronomy conference. The highest velocity material expelled in a cataclysmic, stellar explosion 10 years ago has been detected for the first time by the Hubble telescope's imaging spectrograph. The top image, taken with Hubble's visible-light camera, shows the orange-red rings surrounding Supernova 1987A in the Large Magellanic Cloud. The glowing debris of the supernova explosion, which occurred in February 1987, is at the center of the inner ring. The small, white square indicates the location of the imaging spectrograph aperture. The Hubble data in the middle panel [and a schematic representation in the bottom panel] shows the presence of glowing hydrogen expanding at a speed of 33 million mph (15,000 kilometers per second) coming from an extended area inside the inner ring. |
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Hubble Clicks Images of Io S
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| Title |
Hubble Clicks Images of Io Sweeping across Jupiter |
|
Fireworks of Star Formation
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| Title |
Fireworks of Star Formation Light up a Galaxy |
| General Information |
What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. Back to top [ #top ] |
|
Hubble Reopens Its Eye on th
…
| Title |
Hubble Reopens Its Eye on the Universe |
| General Information |
What is an Early Release Observation? A photograph of a celestial object that demonstrates the performance of a new Hubble camera. Back to top [ #top ] |
|
Star Clusters Born in the Wr
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| Title |
Star Clusters Born in the Wreckage of Cosmic Collisions |
|
A Bow Shock Near a Young Sta
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| Title |
A Bow Shock Near a Young Star |
| General Information |
What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. The Hubble Space Telescope continues to reveal various stunning and intricate treasures that reside within the nearby, intense star-forming region known as the Great Nebula in Orion. One such jewel is the bow shock around the very young star, LL Ori, featured in this Hubble Heritage image. |
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Movies from Hubble Show the
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| Title |
Movies from Hubble Show the Changing Faces of Infant Stars |
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Mars: Closest Encounter
| Title |
Mars: Closest Encounter |
|
Mars: Closest Encounter
| Title |
Mars: Closest Encounter |
|
NASA Space Observatories Gli
…
| Title |
NASA Space Observatories Glimpse Faint Afterglow of Nearby Stellar Explosion |
| General Information |
What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. Back to top [ #top ] |
|
Cassiopeia A - The Colorful
…
| Title |
Cassiopeia A - The Colorful Aftermath of a Violent Stellar Death |
| General Information |
What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. A new image taken with NASA's Hubble Space Telescope provides a detailed look at the tattered remains of a supernova explosion known as Cassiopeia A (Cas A). It is the youngest known remnant from a supernova explosion in the Milky Way. The new Hubble image shows the complex and intricate structure of the star's shattered fragments. The image is a composite made from 18 separate images taken in December 2004 using Hubble's Advanced Camera for Surveys (ACS). |
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Uncovering the Veil Nebula
| Title |
Uncovering the Veil Nebula |
| General Information |
What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. What is a News Nugget? News Nuggets are bulletins from the world of astronomy. NASA's Hubble Space Telescope photographed three magnificent sections of the Veil Nebula -- the shattered remains of a supernova that exploded thousands of years ago. This series of images provides beautifully detailed views of the delicate, wispy structure resulting from this cosmic explosion. The Veil Nebula is one of the most spectacular supernova remnants in the sky. The entire shell spans about 3 degrees on the sky, corresponding to about 6 full moons. |
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Anatomy of a Coronal Hole Th
…
| Description |
Anatomy of a Coronal Hole The south pole of the Sun seen in the light of several ultraviolet spectral lines formed at different temperatures Raster scan images simultaneously obtained in July 1996 by the telescope and spectrometer SUMER (Solar Ultraviolet Measurements of Emitted Radiation) onboard the ESA/NASA Solar and Heliospheric Observatory (SOHO). SUMER was developed at the Max-Planck-Institut f?r Aeronomie (MPAE) as part of an international cooperation. It was financially supported by DLR, CNES, NASA, ESA, MPG and PTB. |
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Western Fires: Fast Approach
…
| Title |
Western Fires: Fast Approach with State Lines |
| Abstract |
Western Fires. Fast Approach with State Lines. August 6, 2000 |
| Completed |
2000-08-07 |
|
TRACE Ultraviolet View of Ja
…
| Title |
TRACE Ultraviolet View of January 20, 2005 Solar Flare |
| Completed |
2005-05-19 |
|
TRACE Ultraviolet View of Ja
…
| Title |
TRACE Ultraviolet View of January 20, 2005 Solar Flare |
| Completed |
2005-05-19 |
|
TRACE Ultraviolet View of Ja
…
| Title |
TRACE Ultraviolet View of January 20, 2005 Solar Flare |
| Completed |
2005-05-19 |
|
TRACE Ultraviolet View of Ja
…
| Title |
TRACE Ultraviolet View of January 20, 2005 Solar Flare |
| Completed |
2005-05-19 |
|
TRACE Ultraviolet View of Ja
…
| Title |
TRACE Ultraviolet View of January 20, 2005 Solar Flare |
| Completed |
2005-05-19 |
|
January 2005 Solar Flares fr
…
| Title |
January 2005 Solar Flares from SOHO/EIT |
| Completed |
2005-05-19 |
|
January 2005 Solar Flares fr
…
| Title |
January 2005 Solar Flares from SOHO/EIT |
| Completed |
2005-05-19 |
|
January 2005 Solar Flares fr
…
| Title |
January 2005 Solar Flares from SOHO/EIT |
| Completed |
2005-05-19 |
|
RHESSI and TRACE View of Jan
…
| Title |
RHESSI and TRACE View of January 20, 2005 Solar Flare |
| Abstract |
RHESSI spacecraft images of gamma-rays (blue) and X-rays (red) thrown off by the hottest part of the flare are shown with UV images from the TRACE spacecraft. The gamma rays are made by energetic protons at the Sun. Scientists were surprised that the gamma rays matched the energy spectrum of protons at Earth: the proton storm may have come directly from the Sun and not from the CME as anticipated. |
| Completed |
2005-05-19 |
|
RHESSI and TRACE View of Jan
…
| Title |
RHESSI and TRACE View of January 20, 2005 Solar Flare |
| Abstract |
RHESSI spacecraft images of gamma-rays (blue) and X-rays (red) thrown off by the hottest part of the flare are shown with UV images from the TRACE spacecraft. The gamma rays are made by energetic protons at the Sun. Scientists were surprised that the gamma rays matched the energy spectrum of protons at Earth: the proton storm may have come directly from the Sun and not from the CME as anticipated. |
| Completed |
2005-05-19 |
|
Galileo Earth Views (WMS)
| Title |
Galileo Earth Views (WMS) |
| Abstract |
The Galileo spacecraft was launched from the Space Shuttle Atlantis on October 18, 1989 on a six-year trip to Jupiter. On the way, the trajectory of the spacecraft took it past Venus once and Earth twice. Galileo took the Earth images in this animation just after the first flyby of the Earth, on December 11 and 12, 1990. This six-hour sequence of images taken two minutes apart clearly shows how the Earth looks from space and how fast (or slow) the cloud features change when looked at from a distance. The path of the sun can be seen crossing Australia by its reflection in the nearby ocean, and the terminator region between night and day can be seen moving across the Indian Ocean. In the original images, the Earth's rotation is so dominant that cloud movement is hard to see, but these images have been mapped to the Earth is such a way that a viewer can watch just the clouds move in the ocean around Antarctica or across the Austrailian land mass. In this animation, New Zealand can ony be seen as a stationary disturbance under a moving cloud bank. The black area with the sharp boundary to the north and east of Australia is the side of the Earth that could not be seen from Galileo's position. |
| Completed |
2004-08-06 |
|
MODIS Mosaic of Antarctica v
…
| Title |
MODIS Mosaic of Antarctica view of Pine Island and Thwaites Glacier without ICESat Topography |
| Abstract |
NASA has released a digital image map of the Antarctic continent and surrounding islands. The Moderate Resolution Imaging Spectroradiometer (MODIS) Mosaic of Antarctica (MOA) image map is a composite of 260 swaths comprised of both Terra and Aqua MODIS images acquired between November 20, 2003 and February 29, 2004. MOA provides a cloud-free view of the ice sheet, ice shelves, and land surfaces at a grid scale of 125 m and an estimated resolution of 150 m. All land areas south of 60° S that are larger than a few hundred meters are included in the mosaic. Also included are several persistent fast ice areas and grounded icebergs. |
| Completed |
2005-11-30 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
Bolivian Deforestation 1984-
…
| Title |
Bolivian Deforestation 1984-1998: Fast Dissolve without Dates |
| Abstract |
These images show deforestation near Santa Cruz, Bolivia from 1984 to 1998. In the initial 1984 scene, some clearing has already occurred in the humid forest and chaparral. The long striped clearings in the center of the scene are predominately from soybean farms created by Mennonite and Japanese farmers. The more circular patterns, appears in a grid pattern to the North (up) and West (left), are government-run and 'national' farms. The scene is roughly 150 miles tall and 200 miles wide. The city of Santa Cruz lies to the west of the river cutting through the scene. |
| Completed |
1999-12-01 |
|
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