Takehiro Miyagoshi and Takaaki Yokoyama 2003 ApJ 593 L133 doi:10.1086/378215
Takehiro Miyagoshi1,3 and Takaaki Yokoyama2,4
Show affiliationsWe studied solar coronal X-ray jets by MHD numerical simulations with thermal conduction effects based on the magnetic reconnection model. Key physical processes are included, such as the emergence of magnetic fluxes from the convection zone, magnetic reconnection with the coronal magnetic fields, heat conduction to the chromosphere, and chromospheric evaporation. High-density evaporation jets were successfully reproduced in the simulations. The mass of the evaporation jets M is described as M = 6.8 × 1012 g(B/10 G)15/7(Tcor/106 K)5/14 × (sflare/5000 km)12/7(t/400 s), where B is the magnetic field strength, Tcor is the coronal temperature, sflare is the loop height, and t is the duration of the ejection.
MHD; Sun: corona; Sun: flares; Sun: magnetic fields; Sun: X-rays, gamma rays
Issue 2 (2003 August 20)
Received 2002 December 17, accepted for publication 2003 July 7
Published 2003 July 16
Takehiro Miyagoshi and Takaaki Yokoyama 2003 ApJ 593 L133
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