3d Simulation Of Time Dependent Emissions From Active-region Coronal Loops*

Details 3d Simulation Of Time Dependent Emissions From Active-region Coronal Loops* 3d Simulation Of Time Dependent Emissions From Active-region Coronal Loops*

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9125m&link_type=abstract

American Astronomical Society Meeting 210, #91.25; Bulletin of the American Astronomical Society, Vol. 39, p.208

Astronomy and Astrophysics

Astronomy

Scientific paper

We investigate the coronal heating mechanism by utilizing the EUV and soft X-ray emissions from plasma loops in active regions. These radiation signatures are believed to be strongly related to the thermal structure of the loops, and therefore can be utilized as diagnostics for the heating mechanism. The very existence of these emitting loops and their formation severely constrain the heating models; namely, an arbitrary heating model may not support a plasma loop in 3D dynamically and thermally with properties consistent with observations. We have identified a class of heating models that can lead to the formation of these loops by solving a modified system of MHD equation supplemented by an energy equation to take into account the heating, radiative cooling and thermal conduction. Additional constraints are imposed by the high-resolution observations from TRACE. Although the loops observed by SXT/Yohkoh (soft X-ray) and EIT/SOHO (EUV) appear to be in a quasi-steady state, data from TRACE (EUV) indicate that the brightness of some loops is time dependent and plasma flows can be present. We scan the parameter space of these heating models and further narrow down the range to those that can reproduce the time dependent emissions which mimic the TRACE images.
*Work supported by Sun-Earth Connection Theory Program of NASA

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