銀河中心領域のフィラメント構造 Ra. Losa et al (2000) VLA Yusef-Zadeh and Morris 1987
降着円盤の大局的3次元MHD シミュレーション Initial Condition :β=1 Machida et al. 2000
Application to Sgr. A* (Machida et al. 2007 in prep) 43 GHz 690 GHz τ=1 surface (3 Dview) 1 AU
銀河ガス円盤のMHDシミュレーション Nishikori, H. , Machida, M. , and Matsumoto, R. , Ap. J 641, 862 (2006)
渦状銀河の平均磁場:起源はダイナモ? M 51 (Neininger & Horellou, 1996) Our Galaxy (Han et al. , 2002)
磁気回転不安定性(MRI) Angular momentum MRI in differentially rotating disks (Balbus and Hawley 1991)
velosity Loop形成のメカニズム velosity position Color: 12 CO Contour: 13 CO(white) position B=100μG 体積=100pc3 個数密度 n= 15 0 cm-3 Emag = 1052 erg アルフベン速度 VA = 24 km s-1
2 D MHD simulations of Parker instability Fukui et al. (2006)
Formation of magnetic loops Magnetic loop structure : plasma β=1 Hight : 400 pc Length : 1 kpc Inclination angle: 40度 Magnetic loops are created where the gas density becomes lower than the region outside the loop. Yellow: Isosurface of β=1 Blue: Magnetic field strength
星間ガスの熱不安定性 圧力 10000 K cooling heating Inoue, Inutsuka, Koyama 2006 30 K 個数密度