A UNIFIED COMPUTATIONAL MODEL FOR SOLAR AND STELLAR FLARES
By J. Allred, A. Kowalski, M. Carlsson. 2015
136 citations recorded by the source corpus.
We present a unified computational framework that can be used to describe impulsive flares on the Sun and on dMe stars. The models assume that the flare impulsive phase is caused by a beam of charged particles that is accelerated in the corona and propagates downward depositing energy and momentum along the way. This rapidly heats the lower stellar atmosphere causing it to explosively expand and dramatically brighten. Our models consist of flux tubes that extend from the sub-photosphere into the corona. We simulate how flare-accelerated charged particles propagate down one-dimensional flux tubes and heat the stellar atmosphere using the Fokker–Planck kinetic theory. Detailed radiative transfer is included so that model predictions can be directly compared with observations. The flux of flare-accelerated particles drives return currents which additionally heat the stellar atmosphere. These effects are also included in our models. We examine the impact of the flare-accelerated particle beams on model solar and dMe stellar atmospheres and perform parameter studies varying the injected particle energy spectra. We find the atmospheric response is strongly dependent on the accelerated particle cutoff energy and spectral index.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/92a5b3204465b9ad96580d79b553d6ff0747a3c6
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In Astronomy and Astrophysics
Citations in the corpus
- THE KEPLER CATALOG OF STELLAR FLARES (2016, background): “Numerical simulations are now able to describe much of the physics for solar and stellar flares and their effect on a star’s atmosphere (Allred et al. 2015).”