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Video footage of the TRACE launch on 1998 April 02, on a Pegasus XL. The L-1011 airplane carrying the rocket took off from Edwards Air Force Base and dropped the rocket over the Pacific Ocean. There rocket thrusters boosted the payload into a Sun-synchronous orbit , from which TRACE gets an uninterrupted view of the Sun for 8 months of the year. | TRACE Launch - April 02 1998 | Color QT Large 21Mb Small 7.3Mb |
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Artist's representation shows the deployment of the solar arrays and opening of the telescope door so that the TRACE instrument can view the Sun. | Solar Array Deployment | Color QT Large 3.8Mb Small 2.6Mb |
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This sequence of ultraviolet images shows dynamic loops at the solar limb. The pattern of moving brightness, showing the flow of mass and/or energy along a series of loops, resembles a jumping fish. | May 8, 1998 1550 Angstrom 60,000 to 250,000 Kelvin |
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This sequence of ultraviolet images shows a flare at the solar limb in a chromospheric line of hydrogen. Hot plasma fills the loops and then falls back down th loops to the limb.A flare is an energetic release of electromagnetic radiation (light) and particles. | May 19, 1998 1216 Angstrom 10,000 to 30,000 Kelvin |
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This sequence of extreme ultraviolet images shows brightening and expansion of coronal loops accompanied by a violent ejection of material away from the Sun's surface. A bubble of hot, ionized gas or plasma as well as cooler, dark filamentary material, erupts from the solar corona and travels through space at a high speed. The cross-shaped pattern at the peak of the loop brightening is an artifact of the instrument response rather than a feature on the Sun. | July 11, 1998 195 Angstrom 500,000 to 2,000,000 Kelvin |
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This sequence of ultraviolet images shows the the same CME/flare event as seen in the chromosphere. The dark region at the center of the activity is a sunspot. | July 11, 1998 1600 Angstrom 4,000 to 10,000 Kelvin |
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This sequence of extreme ultraviolet images shows several concentrations of dark filamentary material dancing along the solar limb, against a background of brightening coronal loops. Filamentary material is cool plasma that is supported by magnetic fields above the photosphere. They appear dark when seen against the bright solar disk. Filaments such as this one that are seen on the limb are called prominences. | July 27, 1998 171 Angstrom 160,000 to 2,000,000 Kelvin |
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This sequence of extreme ultraviolet images shows the effect of a moderate size (GOES class M) flare on a set of active region loops on the solar disk. The bright crosses seen at the peak of the flare are an artifact of the instrument response not a solar phenomenon. The violent release of energy causes many of the loops to oscillate as well as producing or activating many post flare loops not visible before the event. | July 14, 1998 171 Angstrom 160,000 to 2,000,000 Kelvin |
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This sequence of extreme ultraviolet images shows the dynamic interactions of neighboring active regions. There are flows and brightenings and a lot of other activity but no actual flares. An active region is an area on the Sun with a large concentration of magnetic field, often containing sunspots and sometimes producing flares. | August 19, 1998 171 Angstrom 160,000 to 2,000,000 Kelvin |
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This sequence of extreme ultraviolet images shows a filigree or moss-like structure. Moss has been found to be cooler and lower lying than most of the coronal material, and appear to be associated with the footpoints of loops. | August 1, 1999 195 Angstrom 500,000 to 2,000,000 Kelvin |
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This spectacular sequence of EUV images shows graceful motion and evolution of a cluster of loops at the limb. | August 09, 1999 171 Angstrom 160,000 to 2,000,000 Kelvin |
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This sequence of EUV images shows cool filamentary material erupting and moving outwards from the Sun, leaving behind a set of hotter, brighter, activated coronal loops. | October 20, 1999 195 Angstrom 500,000 to 2,000,000 Kelvin |
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