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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. 9.

Unstable regions in the disks with various power indices for the surface density: (a) ﹩q=2﹩, ﹩\Sigma _{0}=4.8\times 10^{3}﹩ g cm﹩^{-2}﹩, (b) ﹩q=3/2﹩, ﹩\Sigma _{0}=1.7\times 10^{3}﹩ g cm﹩^{-2}﹩, (c) ﹩q=1﹩, ﹩\Sigma _{0}=3.3\times 10^{2}﹩ g cm﹩^{-2}﹩, and (d) ﹩q=0﹩, ﹩\Sigma _{0}=6.6﹩ g cm﹩^{-2}﹩. The other parameters are the same as those of the fiducial model. All these models have the same disk mass 0.024 ﹩M_{\odot }﹩ between 0.1 and 100 AU. The solid and dashed curves represent the loci of ﹩\lambda _{\mathrm{res}\,}/ H=1﹩ for the cases of the field strength ﹩\beta _{c}=100﹩ and 1000, respectively, inside of which is magnetorotationally stable. The dotted curve represents the scale height of the disk ﹩z=H( r) ﹩.

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