Radiative Signatures of the Coronal Heating and Cooling Cycle

Details Radiative Signatures of the Coronal Heating and Cooling Cycle Radiative Signatures of the Coronal Heating and Cooling Cycle

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.0503b&link_type=abstract

American Astronomical Society, SPD meeting #42, #5.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

The 'smoking gun' of small-scale, impulsive heating in the non-flaring solar corona is expected to be emission from plasma at temperatures greater than 5 MK. Recent studies, designed to strongly constrain the high temperature part of the emission measure distribution, have begun to provide evidence for such a hot component to the emission spectrum. However, it is significantly weaker than predicted by numerical models. We propose that the discrepancy can be resolved by dropping the common modeling assumption of ionization equilibrium.
The launches of Hinode and the Solar Dynamics Observatory (SDO) have brought the matter of the ionization state of the plasma, which lies at the interface between models and observations, firmly to the forefront.
We present detailed, quantitative predictions for the spectral emission that the instruments EIS and AIA would actually detect, for a broad range of impulsive heating scenarios, derived from a combination of numerical hydrodynamic and forward modeling.
We demonstrate that a nonequilibrium ionization state, as induced by small-scale, impulsive heating, leads to predictions for observable quantities that are consistent with what is actually observed.

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