Heating Constraints on the Solar Corona Determined from SERTS Observations

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Session 59 -- Solar Surface and Corona
Oral presentation, Thursday, January 13, 10:15-11:45, Salon VI Room (Crystal Gateway)

[59.05] Heating Constraints on the Solar Corona Determined from SERTS Observations

D.A. Falconer (University of Maryland, NASA/GSFC), J.M. Davila, R.J. Thomas (NASA/GSFC), W.T. Thompson$^*$ (NASA/GSFC)

\par EUV emission above the quiet solar limb up to 1.2$R_{\odot}$ was studied using observations made from two different flights of the Goddard Solar EUV Rocket Telescope and Spectrograph (SERTS) covering three different spatial locations. \par The spectral line intensities from a number of EUV spectral lines as a function of height were analyzed. Ratio of iron line intensities from Fe XIII, Fe XIV, Fe XV and Fe XVI were used to determine the electron temperature. The emission measure was determined from the iron line intensities and the electron temperature. Since in all three cases the line ratio temperature increased with height, a source of heating is required at some location above the maximum observed height, which was 1.15$R_{\odot}$ for two locations and 1.2$R_{\odot}$ for the third location. \par The maximum divergence of heat flux was determined from the variation of temperature versus radius. The total radiatiative power was obtained from the emission measure and temperature. By comparing the divergence of heat flux and the total radiatiative power, heating was also shown to be necessary for two of the three cases throughout the region below 1.15$R_{\odot}$.


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