A Simulation of Protostar Flares and the Expected X-Ray Spectrum

Details A Simulation of Protostar Flares and the Expected X-Ray Spectrum A Simulation of Protostar Flares and the Expected X-Ray Spectrum

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..362..304k&link_type=abstract

The Seventh Pacific Rim Conference on Stellar Astrophysics, ASP Conference Series, Vol. 362, Proceedings of the conference held

Astronomy and Astrophysics

Astrophysics

Scientific paper

We performed one-dimensional hydrodynamic simulations of flare loops on protostars by applying the reconnection model for a solar flare. A magnetic loop from the central star that penetrates an accretion disk was assumed. We found that the plasma in the loop was heated by conduction, and that evaporation of the disk matter made the plasma denser. This effect was seen only in the half-loop on the reconnection side. The hard X-ray spectrum expected from our simulation has a shape very similar to the solar one observed by RHESSI}, except that the energy band (sim200 keV) is 10 times higher than that of the solar flare.

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