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Transition Region Emission and the Energy Input to Thermal Plasma in Solar FlaresUnderstanding the energetics of solar flares depends on obtaining reliable determinations of the energy input to flare plasma. X-ray observations of the thermal bremsstrahlung from hot flare plasma provide temperatures and emission measures which, along with estimates of the plasma volume, allow the energy content of this hot plasma to be computed. However, if thermal energy losses are significant or if significant energy goes directly into cooler plasma, this is only a lower limit on the total energy injected into thermal plasma during the flare. We use SOHO UVCS observations of O VI flare emission scattered by coronal O VI ions to deduce the flare emission at transition region temperatures between 100,000 K and 1 MK for the 2002 July 23 and other flares. We find that the radiated energy at these temperatures significantly increases the deduced energy input to the thermal plasma, but by an amount that is less than the uncertainty in the computed energies. Comparisons of computed thermal and nonthermal electron energies deduced from RHESSI, GOES, and UVCS are shown.
Document ID
20050177219
Document Type
Conference Paper
Authors
Holman, Gordon D.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Holman, Gordon D.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Dennis, Brian R.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Haga, Leah
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Raymond, John C.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Panasyuk, Alexander
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 23, 2013
Publication Date
January 1, 2005
Subject Category
Solar Physics
Report/Patent Number
AGU-61006-121
Meeting Information
AGU/SPD Meeting(New Orleans, LA)
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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