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IBEX Heliosphere Map - 2.8 to 5.6 keV
IBEX Heliosphere Map - ...
10/15/09
Southwest Research Inst...
 
Year 2009
IBEX Heliosphere Map - 0.6 to 1.0 keV
IBEX Heliosphere Map - ...
10/15/09
Southwest Research Inst...
 
Year 2009
IBEX Heliosphere Map - 1.3 to 2.4 keV
IBEX Heliosphere Map - ...
10/15/09
Southwest Research Inst...
 
Year 2009
IBEX Heliosphere Map - 1.9 to 3.6 keV
IBEX Heliosphere Map - ...
10/15/09
Southwest Research Inst...
 
Year 2009
IBEX Heliosphere Map - 0.9 to 1.5 keV
IBEX Heliosphere Map - ...
10/15/09
Southwest Research Inst...
 
Year 2009
Lockheed Fire
Lockheed Fire
8/18/09
NASA
 
Year 2009
LCROSS
LCROSS
2/24/09
NASA
 
Year 2009
Stennis personnel participate in test program
Stennis personnel parti...
Fernando Figueroa, John...
9/9/08
NASA/Stennis Space Cent...
 
Year 2008
Voyager 2
Voyager 2
4/2/90
NASA/JPL-Caltech
 
Year 1990
6/16/05
NASA/JPL-Caltech
 
Year 1905
Multi-angle Images of Hudson Bay and James Bay, Canada
Multi-angle Images of H...
NASA/JPL-Caltech
 
Nine Frames as Jupiter Turns
Nine Frames as Jupiter ...
11/6/00
NASA/JPL-Caltech
 
Year 2000
Rossby Waves TOPEX/Poseidon
Rossby Waves TOPEX/Pose...
4/12/96
NASA/JPL-Caltech
 
Year 1996
Gamma-Ray Burst 050525a
 
Stars Can't Spin Out of...
 
Neptune
Neptune
Image
08.21.1989
 
Full-Disk Neptune
Full-Disk Neptune
Image
08.20.1989
 
MOLA: Seasonal Snow Variations on Mars, Fast Zoom out from Martian South Pole: False Color
MOLA: Seasonal Snow Var...
MGS/MOLA
Topography of the south...
 
MOLA: Seasonal Snow Variations on Mars, Fast Zoom out from Martian South Pole: False Color
MOLA: Seasonal Snow Var...
MGS/MOLA
None
 
MOLA: Seasonal Snow Variations on Mars: Fast Zoom to Martian North Pole: False Color
MOLA: Seasonal Snow Var...
MGS/MOLA
Topography of the north...
 
MOLA: Seasonal Snow Variations on Mars: Fast Zoom to Martian North Pole: False Color
MOLA: Seasonal Snow Var...
MGS/MOLA
None
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
September 8, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
Oct 10, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
October 26, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
November 4, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
November 9, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
November 11, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
November 12, 2001
 
Pine Island Iceberg Formation
Pine Island Iceberg For...
RADARSAT-1/SAR
None
 
MOLA Zooming Down to Reveal a Hidden Channel (fast version)
MOLA Zooming Down to Re...
MGS/MOLA
In this visualization, ...
 
TRACE Observes Flows over Active Regions (Fast play)
TRACE Observes Flows ov...
SOHO/EIT
Full-disk view of the S...
 
TRACE Observes Flows over Active Regions (Fast play)
TRACE Observes Flows ov...
SOHO/EIT
Close-up view of the ou...
 
TRACE Observes Flows over Active Regions (Fast play)
TRACE Observes Flows ov...
SOHO/EIT
None
 
Neptune Full Disk View
Neptune Full Disk View
Planet-Neptune
04/02/1990
NASA
 
NASA Center Jet Propulsion Laboratory
A coronal mass ejection (CME)on August 16, 2001, is captured by the LASCO C2 instrument as it first erupts (left). Just over an hour later in a wider view from LASCO C3 the CME is also accompanied by fast, high energy protons that have struck the SOHO spacecraft's detectors. This larger view encompasses 30 times the radius of the Sun.
A coronal mass ejection...
Image
 
Description A coronal mass ejection (CME)on August 16, 2001, is captured by the LASCO C2 instrument as it first erupts (left). Just over an hour later in a wider view from LASCO C3 the CME is also accompanied by fast, high energy protons that have struck the SOHO spacecraft's detectors. This larger view encompasses 30 times the radius of the Sun.
Sequence of SOHO-EIT first difference images showing the intensity (density) enhancement and following rarefaction associated with a shock wave expanding across the solar disk from the site of the origin of a coronal mass ejection (CME), 1997 May 12. A halo CME was observed by SOHO-LASCO. These images were formed from the differences of successive images in the emission lines of Fe XII near 195 A; this ion is formed at temperatures of about 1.5 million degrees. The wave front travels at speeds of ~ 300 km/s, typical of a fast mode Alfv?n shock in the lower solar corona.
Sequence of SOHO-EIT fi...
Image
 
Description Sequence of SOHO-EIT first difference images showing the intensity (density) enhancement and following rarefaction associated with a shock wave expanding across the solar disk from the site of the origin of a coronal mass ejection (CME), 1997 May 12. A halo CME was observed by SOHO-LASCO. These images were formed from the differences of successive images in the emission lines of Fe XII near 195 A; this ion is formed at temperatures of about 1.5 million degrees. The wave front travels at speeds of ~ 300 km/s, typical of a fast mode Alfv?n shock in the lower solar corona.
Sequence of SOHO-EIT images showing a shock wave expanding across the solar disk from the site of the origin of a coronal mass ejection (CME), 1997 May 12. A halo CME was observed by SOHO-LASCO. EIT recorded these images in the emission lines of Fe XII near 195 A; this ion is formed at temperatures of about 1.5 million degrees. The wave front travels at speeds of ~ 300 km/s, typical of a fast mode Alfv?n shock in the lower solar corona.
Sequence of SOHO-EIT im...
Image
 
Description Sequence of SOHO-EIT images showing a shock wave expanding across the solar disk from the site of the origin of a coronal mass ejection (CME), 1997 May 12. A halo CME was observed by SOHO-LASCO. EIT recorded these images in the emission lines of Fe XII near 195 A; this ion is formed at temperatures of about 1.5 million degrees. The wave front travels at speeds of ~ 300 km/s, typical of a fast mode Alfv?n shock in the lower solar corona.
SOLAR ROTATION RATE WITH DEPTH IMAGE: This image, taken using the Michelson Doppler Imager (MDI) instrument on board the NASA/ESA Solar and Heliospheric Observatory (SOHO) spacecraft, shows differences in the speed of rotation of material in the Sun. This image is made from continuous observations over a period of twelve months beginning in May 1996. The false colors represent speed; red material is rotating the fastest, dark blue, the slowest. The left side of the figure is rotation speed at the surface of the Sun; red material at the equator is moving approximately three thousand miles per hour faster than the blue material at the poles. The cutaway on the right reveals rotation speed inside the Sun. The large dark red band is a massive fast flow of hot, electrically charged gas called plasma beneath the solar equator. This plasma stream is approximately 300 thousand miles wide and 130 thousand miles deep. This material moves about four percent faster than the surrounding material. Additionally, the newly discovered, but much more subtle, plasma streams can be seen in the cutaway at the poles. They are the light blue areas embedded in the slower moving dark blue regions. Although much smaller than the equatorial stream, they are still immense by terrestrial standards. Each stream is about 17,000 miles across, large enough to engulf two Earths. This material moves about ten percent faster than its surroundings. (Photo Credit: Stanford University)
SOLAR ROTATION RATE WIT...
Image
 
Description SOLAR ROTATION RATE WITH DEPTH IMAGE: This image, taken using the Michelson Doppler Imager (MDI) instrument on board the NASA/ESA Solar and Heliospheric Observatory (SOHO) spacecraft, shows differences in the speed of rotation of material in the Sun. This image is made from continuous observations over a period of twelve months beginning in May 1996. The false colors represent speed; red material is rotating the fastest, dark blue, the slowest. The left side of the figure is rotation speed at the surface of the Sun; red material at the equator is moving approximately three thousand miles per hour faster than the blue material at the poles. The cutaway on the right reveals rotation speed inside the Sun. The large dark red band is a massive fast flow of hot, electrically charged gas called plasma beneath the solar equator. This plasma stream is approximately 300 thousand miles wide and 130 thousand miles deep. This material moves about four percent faster than the surrounding material. Additionally, the newly discovered, but much more subtle, plasma streams can be seen in the cutaway at the poles. They are the light blue areas embedded in the slower moving dark blue regions. Although much smaller than the equatorial stream, they are still immense by terrestrial standards. Each stream is about 17,000 miles across, large enough to engulf two Earths. This material moves about ten percent faster than its surroundings. (Photo Credit: Stanford University)
MDI Sunspot size winner -- Active region 10486 became the largest sunspot seen by SOHO, It unleashed a spectacular show on 28 October 2003. An X 17.2 flare, the second largest flare observed by SOHO and the third largest ever recorded, blasted off a strong high energy proton event and a fast-moving Coronal Mass Ejection. The spot occupied an area equal to about 15 Earths, a size not seen since 1989. It later fired off the largest X-ray flare recorded, on 4 November 2003.
MDI Sunspot size winner...
Image
 
Description MDI Sunspot size winner -- Active region 10486 became the largest sunspot seen by SOHO, It unleashed a spectacular show on 28 October 2003. An X 17.2 flare, the second largest flare observed by SOHO and the third largest ever recorded, blasted off a strong high energy proton event and a fast-moving Coronal Mass Ejection. The spot occupied an area equal to about 15 Earths, a size not seen since 1989. It later fired off the largest X-ray flare recorded, on 4 November 2003.
SURFING THE SOLAR WIND - The outermost solar atmosphere, or corona, is normally visible only during a solar eclipse. New observations of particles ``surfing'' on waves in the corona have shed light on an ongoing mystery of why the solar wind flows as fast as it does. Charged particles in the solar wind spiral around lines of magnetic force, and these lines oscillate back and forth to create outward-propagating waves. When the particles' spiraling frequencies match the wave frequencies, the particles can absorb the waves' energy; this spins up the particles into larger orbits, gives them an added outward boost, and damps out the waves. (Image credit: NASA/Dana Berry, Allied Signal Max Q digital animation group)
SURFING THE SOLAR WIND ...
Image
 
Description SURFING THE SOLAR WIND - The outermost solar atmosphere, or corona, is normally visible only during a solar eclipse. New observations of particles ``surfing'' on waves in the corona have shed light on an ongoing mystery of why the solar wind flows as fast as it does. Charged particles in the solar wind spiral around lines of magnetic force, and these lines oscillate back and forth to create outward-propagating waves. When the particles' spiraling frequencies match the wave frequencies, the particles can absorb the waves' energy; this spins up the particles into larger orbits, gives them an added outward boost, and damps out the waves. (Image credit: NASA/Dana Berry, Allied Signal Max Q digital animation group)
AC96-0058-1
AC96-0058-1
2/13/96
NASA/Ames Research Cent...
 
Year 1996
AC96-0058-2
AC96-0058-2
2/13/96
NASA/Ames Research Cent...
 
Year 1996
AC96-0058-3
AC96-0058-3
2/13/96
NASA/Ames Research Cent...
 
Year 1996
AC96-0058-4
AC96-0058-4
2/13/96
NASA/Ames Research Cent...
 
Year 1996
AC96-0058-5
AC96-0058-5
2/13/96
NASA/Ames Research Cent...
 
Year 1996
AC96-0058-6
AC96-0058-6
2/13/96
NASA/Ames Research Cent...
 
Year 1996
AC96-0058-7
AC96-0058-7
2/13/96
NASA/Ames Research Cent...
 
Year 1996
Revelations
Revelations
2008-02-14 0:0:0
 
The "Rotten Egg" Nebula: A Planetary Nebula in the Making
The "Rotten Egg" Nebula...
OH231.8+4.2
2008-02-15 0:0:0
 
Supernova Survivor: First Supernova Companion Star Found
Supernova Survivor: Fir...
2008-02-15 0:0:0
 
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