Solar Flare Model Atmospheres

Details Solar Flare Model Atmospheres Solar Flare Model Atmospheres

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4101f&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #41.01; Bulletin of the American Astronomical Society, Vol. 24, p.794

Astronomy and Astrophysics

Astronomy

Scientific paper

We present 3 sets of solar flare atmospheric models, computed in 3 different limits. In all of the models, energy balance is assumed, with radiative losses from the optically thick transitions of HI, CaII, and MgII balancing flare heating from nonthermal electrons and X-rays from the flaring corona. In the ``Hydrostatic'' models, we have assumed that flare heating by Coulomb collisions from a flux of nonthermal electrons has been occurring for an infinitely long time, and the corona and chromosphere have achieved both energetic and hydrostatic equilibrium. In the ``Impulsive'' models, we have assumed that the atmospheric density remains frozen in its preflare state, but that the atmosphere rapidly achieves a temperature structure consistent with energy balance. In the ``Evolving'' models, we have assumed a temporal variation of the nonthermal electron heating rate consistent with flare heating for timescales of 5-10 minutes, corresponding to a long lived and intense flare, continually undergoing chromospheric evaporation. In this case, the chromospheric model is in hydrostatic equilibrium, but the flare transition region is at depths that are much less than those in the ``Hydrostatic'' models. We present temperature and density structures in these model atmospheres, line and continuum fluxes from each model, and a few selected line profiles. G.H.F. is supported by AFOSR grant AFOSR-91-116, NASA grant NAGW-2969, and NSF grant ATM91-06052. S.L.H. is supported in part by a Hubble Fellowship from STSI, and in part by Lawrence Livermore National Laboratory. Lawrence Livermore is supported by the US Department of Energy under contract number W-7405-ENG-48.

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