Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh13a..06w&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH13A-06
Astronomy and Astrophysics
Astrophysics
[7500] Solar Physics, Astrophysics, And Astronomy, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7538] Solar Physics, Astrophysics, And Astronomy / Solar Irradiance, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions
Scientific paper
Much of our current understanding of the temperature and density structure of solar flares has been derived from broad band X-ray instruments, such as RHESSI, GOES, and SXT/Yohkoh, or the observation of isolated emission lines, such as from BCS/Yohkoh. This has lead to uncertainties in determining the distribution of temperatures and densities in a flare. The EUV Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO) provides an unprecedented opportunity to observe a very wide range of high-temperature emission lines at high cadence (10 s) and relatively high spectral resolution (1 A). The spectral range between 90 and 200 Angstroms is particularly rich in emission lines from Fe that are formed at temperatures above 7 MK (Fe XVIII - Fe XXIV). This range also includes one of the few density diagnostics (Fe XXI 145.66/128.75) that is useful in solar flare observations. Our initial calculations suggest very broad differential emission measure distributions and indicate high densities (Log Ne as high as 11.7), which implies a very rapid cooling of flare plasma. These observations are broadly consistent with flare models that allow for the release of energy on many independent threads and we will discuss these results in the context of current theories of solar flares.
Doschek George A.
Eve Team
Mariska John T.
Warren Harry P.
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