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Magnetohydrodynamic Simulations of Accretion Disksaround a Weakly Magnetized Neutron Star in StrongGravity 

作成者 松元, 亮治
キーワード等 accretion, magnetohydrodynamic
日本十進分類法 (NDC) 440
内容 We carried out two dimensional high-resolution magnetohydrodynamic (MHD) simulations of an accretiondisk around a weakly magnetized neutron star. General relativistic eects are taken into account by usingpseudo-Newtonian potential of Pacz´ynski, B., P. J. Witta (1980). When magnetic loops connect the neutronstar and the accretion disk, the twist injection from the disk or from the rotating neutron star triggersexpansion of the loops. Since the expanding magnetic loops prevent inflow toward the magnetic poles of theneutron star, disk matter accumulates on the boundary between the magnetosphere and the disk. Magneticreconnection taking place in the loops creates a channel along which the disk matter can accrete and unloadsthe magnetosphere. This process produces quasi-periodic variation of the accretion flow in the innermostregion of the disk. We found two kinds of oscillations. One is the magnetospheric oscillation regulated bymagnetic reconnection. The other is the radial disk oscillation. The typical frequency of the oscillations is100 Hz to 2 kHz. Furthermore, we predict that QPO sources inevitably accompany X-ray flares by magneticreconnection and bipolar outflows of hot X-ray emitting plasma similar to the optical jets in protostars.
作成日付 2001-04
コンテンツの種類 プレプリント Preprint
DCMI資源タイプ text
ファイル形式 application/pdf
ハンドルURL http://mitizane.ll.chiba-u.jp/meta-bin/mt-pdetail.cgi?cd=00020207
フルテキストへのリンク http://mitizane.ll.chiba-u.jp/metadb/up/joho/matsumoto_0104130X.pdf
言語 英語
著者版フラグ author


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