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Magnetorotational Instability in Protoplanetary Disks. II. Ionization State and Unstable Regions

  • Authors: Takayoshi Sano, Shoken M. Miyama, Toyoharu Umebayashi, and Takenori Nakano

Sano et al. 2000 The Astrophysical Journal 543 486.

  • Provider: AAS Journals

Caption: Fig. 7.

Unstable regions (striped) for the cases of (a) the plasma beta at the midplane ﹩\beta _{c}=100﹩ and (b) ﹩\beta _{c}=1000﹩ for the fiducial model (same as in Fig. 1). The dotted curve denotes the scale height of the disk, ﹩z=H( r) ﹩. In the region above the curve ﹩\lambda _{\mathrm{ideal}\,}/ H=1﹩, the instability does not effectively work because the wavelengths of the unstable modes are larger than the scale height of the disk. The region below the curve ﹩\lambda _{\mathrm{res}\,}/ H=1﹩ is stable because the magnetic dissipation is effective and corresponds to Gammie’s (1996) "dead zone."

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