Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsa41a..04r&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SA41A-04
Physics
2423 Ionization Mechanisms, 2459 Planetary Ionospheres (5435, 5729, 6026, 6027, 6028), 2479 Solar Radiation And Cosmic Ray Effects, 7538 Solar Irradiance, 7554 X Rays, Gamma Rays, And Neutrinos
Scientific paper
Solar soft X-ray irradiance provides a highly variable energy source to the lower thermosphere. Solar flares are a dramatic source of this variability. Observations from the NASA satellite mission Thermosphere, Ionosphere, Mesosphere, Energetics and Dynamics - Solar Extreme Ultraviolet Experiment (TIMED-SEE) are being analyzed to determine how the solar soft X-ray energy deposition varies during a solar flare. The XUV Photometer System (XPS) aboard TIMED-SEE observes the solar soft X-ray irradiance between 0.1 and 27 nm for a 3 minute period approximately every 96 minutes. Contrary to initial assumptions based on the nature and infrequency of solar flares, XPS observations have shown that flares significantly impact the daily averaged energy input and thus the atmospheric chemistry of the lower thermosphere. The XPS observed, on average, eight solar flares of various strengths per month during a five month period in 2002 while the Student Nitric Oxide Explorer (SNOE) observed nitric oxide (NO) between 95 and 135 km. It has been shown that SNOE observed a significant increase in NO during the April 21, 2002 solar flare that was observed by the XPS. The eight XPS photodiodes are broadband detectors and a reference spectrum is required to interpret the signal because the sensitivity varies within each detector bandpass. A solar flare spectrum is inferred from the XPS detectors by an algorithm that iterates through differential emission measures until they produce a model spectrum that can reproduce the XPS detector observations. These flare spectra will be used to determine the soft X-ray energy input to Earth's lower thermosphere during a solar flare. Results and a description of this analysis will be presented.
Bailey Scott M.
Eparvier Francis G.
Rodgers Erica M.
Woods Thomas N.
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