Magnetohydrodynamic Simulations of Hard X-Ray Emission and Mass Outflows from Protostars

Details Magnetohydrodynamic Simulations of Hard X-Ray Emission and Mass Outflows from Protostars Magnetohydrodynamic Simulations of Hard X-Ray Emission and Mass Outflows from Protostars

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..288h&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Physics

1

Scientific paper

We carried out 2.5 dimensional magnetohydrodynamic (MHD) simulations of the magnetic interaction between a protostar and its surrounding disk. The results show that high-velocity and high-temperature plasma flows can be created via magnetic reconnection. In our model which can explain protostellar flares and mass outflows both qualitatively and quantitatively, magnetic reconnection plays an essential role in heating the plasmas. We analyse the one-dimensional distribution across the shock around the reconnection site to clarify the heating machanism in protostellar flares. Around the reconnection point, we found two peaks of peaks of toroidal current density and a pressure increase with decreasing the magnetic field strength, indicating that these shocks are slow-mode shocks

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