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Bibliographic Record
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- Material Type
- 文書・図像類
- Author/Editor
- 松元, 亮治
- Author Heading
- Text Language Code
- eng
- Subject Heading
- NDC
- Target Audience
- 一般
- Note (General)
- type:textWe propose a model of hard X-ray ares in protostars observed by ASCAsatellite. Assuming that the dipole magnetic eld of the protostar threads theprotostellar disk, we carried out 2.5-dimensional magnetohydrodynamic (MHD)simulations of the disk-star interaction. The closed magnetic loops connectingthe central star and the disk are twisted by the rotation of the disk. As thetwist accumulates, magnetic loops expand and nally approach to the open eldconguration. A current sheet is formed inside the expanding loops. In thepresence of resistivity, magnetic reconnection takes place in the current sheet.Outgoing magnetic island and post are loops are formed as a result of thereconnection. The time scale of this `are' is the order of the rotation periodof the disk. The released magnetic energy partly goes into the thermal energyand heats up the aring plasma up to 108 K. The length of the aring loopis several times of the radius of the central star, consistent with observations.The speed of the hot plasmoid ejected by the reconnection is 200 when the footpoint of the loop is at 0.03 AU from 1 M protostar. The hotplasma outow can explain the speed and mass ow rate of optical jets. Dense,cold, magnetically accelerated wind (v 150
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