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X28 flare in EIT 195 -- The Sun unleashed a powerful flare on 4 November 2003 that could be the most powerful ever witnessed and probably as strong as anything detected since satellites were able to record these events n the mid-1970s. The still and video clip from the Extreme ultraviolet Imager in the 195A emission line captured the event. The two strongest flares on record, in 1989 and 2001, were rated at X20. This one was stronger scientists say. But because it saturated the X-ray detector aboard NOAA's GOES satellite that monitors the Sun, it is not possible to tell exactly how large it was. The consensus by scientists put it somewhere around X28.
X28 flare in EIT 195 --...
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Description
X28 flare in EIT 195 -- The Sun unleashed a powerful flare on 4 November 2003 that could be the most powerful ever witnessed and probably as strong as anything detected since satellites were able to record these events n the mid-1970s. The still and video clip from the Extreme ultraviolet Imager in the 195A emission line captured the event. The two strongest flares on record, in 1989 and 2001, were rated at X20. This one was stronger scientists say. But because it saturated the X-ray detector aboard NOAA's GOES satellite that monitors the Sun, it is not possible to tell exactly how large it was. The consensus by scientists put it somewhere around X28.
VARIATIONS IN SOLAR MOTION IMAGE: This image is taken using the Michelson Doppler Imager (MDI) instrument on the NASA/ESA Solar and Heliospheric Observatory (SOHO) spacecraft. It is a result of computations using observations taken continuously from May 1996 to May 1997. This false color image represents the difference in speeds between various areas on the Sun, both at the surface and in the interior. Red - yellow is faster than average and blue is slower than average. On the left side of the image, the light orange bands are zones that are moving slightly faster than their surroundings. The new SOHO observations indicate that these extend down approximately 12,000 miles into the sun. Sunspots, caused by disturbances in the solar magnetic field, tend to form at the edge of these bands. Scientists at the Stanford University, Calif. Solar Oscillations Investigation (SOI) group speculate that this may be due to the difference in speed at the edge of these zones that tend to ?twist? the magnetic field generated by the moving hot, electrically charged gas called plasma. The cutaway on the right side of the image reveals speed variations in the interior of the Sun. Only the outer 30 percent of the Sun?s interior where the variations are more certain is shown. The red ovals embedded in the green areas at the poles are the newly discovered polar plasma ?jet streams?. They move approximately ten percent faster than their surroundings, and each is about 17,000 miles across, large enough to engulf two Earths. (Photo Credit: Stanford University)
VARIATIONS IN SOLAR MOT...
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Description
VARIATIONS IN SOLAR MOTION IMAGE: This image is taken using the Michelson Doppler Imager (MDI) instrument on the NASA/ESA Solar and Heliospheric Observatory (SOHO) spacecraft. It is a result of computations using observations taken continuously from May 1996 to May 1997. This false color image represents the difference in speeds between various areas on the Sun, both at the surface and in the interior. Red - yellow is faster than average and blue is slower than average. On the left side of the image, the light orange bands are zones that are moving slightly faster than their surroundings. The new SOHO observations indicate that these extend down approximately 12,000 miles into the sun. Sunspots, caused by disturbances in the solar magnetic field, tend to form at the edge of these bands. Scientists at the Stanford University, Calif. Solar Oscillations Investigation (SOI) group speculate that this may be due to the difference in speed at the edge of these zones that tend to ?twist? the magnetic field generated by the moving hot, electrically charged gas called plasma. The cutaway on the right side of the image reveals speed variations in the interior of the Sun. Only the outer 30 percent of the Sun?s interior where the variations are more certain is shown. The red ovals embedded in the green areas at the poles are the newly discovered polar plasma ?jet streams?. They move approximately ten percent faster than their surroundings, and each is about 17,000 miles across, large enough to engulf two Earths. (Photo Credit: Stanford University)
A rapidly expanding "solar quake" on the Sun?s surface depicted here by the Michelson Doppler Imager (MDI). It immediately followed a solar flare on 1996 July 6 and spread out more than 100,000 km at the solar surface. Scientists have shown that solar flares produce seismic waves, and gigantic seismic quakes, in the Sun's interior. They have tracked these seismic waves and found that "sun-quakes" closely resemble earthquakes on our planet.
A rapidly expanding "so...
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Description
A rapidly expanding "solar quake" on the Sun?s surface depicted here by the Michelson Doppler Imager (MDI). It immediately followed a solar flare on 1996 July 6 and spread out more than 100,000 km at the solar surface. Scientists have shown that solar flares produce seismic waves, and gigantic seismic quakes, in the Sun's interior. They have tracked these seismic waves and found that "sun-quakes" closely resemble earthquakes on our planet.
POLAR FLOWS IMAGE: This image is a graphical representation of the surface flow from the equator to the poles of the Sun. The flow lines overlay an image of the rotation speed at the Sun?s surface, taken using the Michelson Doppler Imager (MDI) instrument on the NASA/ESA Solar and Heliospheric Observatory (SOHO) spacecraft over a period of 12 months ending June 1997. The false colors represent speed; red material is rotating faster than the blue material. As this material rotates, it is also flowing toward the poles at a relatively slow velocity of about 50 miles per hour. The lines represent how this motion would appear if you could stand on the surface of the Sun about 30 degrees from the equator, and move with the same speed as the material there. If you were at this position in the northern hemisphere, material closer to the equator would appear to move to the right of the image as it flowed north, because it is rotating faster. Material closer to the north pole would appear to move to the left as it flowed north, because it is rotating slower. The cutaway on the left of the image represents the observed polar flow 15 thousand miles beneath the surface and a hypothetical, slower moving return flow from the poles to the equator, estimated to be 120 thousand miles beneath the surface. (Photo Credit: Stanford University)
POLAR FLOWS IMAGE: This...
Image
 
Description
POLAR FLOWS IMAGE: This image is a graphical representation of the surface flow from the equator to the poles of the Sun. The flow lines overlay an image of the rotation speed at the Sun?s surface, taken using the Michelson Doppler Imager (MDI) instrument on the NASA/ESA Solar and Heliospheric Observatory (SOHO) spacecraft over a period of 12 months ending June 1997. The false colors represent speed; red material is rotating faster than the blue material. As this material rotates, it is also flowing toward the poles at a relatively slow velocity of about 50 miles per hour. The lines represent how this motion would appear if you could stand on the surface of the Sun about 30 degrees from the equator, and move with the same speed as the material there. If you were at this position in the northern hemisphere, material closer to the equator would appear to move to the right of the image as it flowed north, because it is rotating faster. Material closer to the north pole would appear to move to the left as it flowed north, because it is rotating slower. The cutaway on the left of the image represents the observed polar flow 15 thousand miles beneath the surface and a hypothetical, slower moving return flow from the poles to the equator, estimated to be 120 thousand miles beneath the surface. (Photo Credit: Stanford University)
More Images of NGC 1569
 
More Images of NGC 1569
 
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