Physics
Scientific paper
Sep 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983pthph..70..747n&link_type=abstract
Progress of Theoretical Physics, Vol. 70, No. 3, pp. 747-756
Physics
6
Scientific paper
The gravitational instability is investigated for a rigidly rotating isothermal gaseous disks with magnetic field whose mean direction is parallel to the rotation axis. It is found that the stability of the disk depends on two non-dimensional parameters p2 ≡ B02/ (4 π2G σ02) and q2 ≡ Ω02/ (π G ρ0c) where B0, σ0, Ω0 and ρ0c are the magnetic field strength, the column density of the disk, the uniform angular velocity and the central density, respectively. The critical value of p2 when the disk is marginally stable is determined as a function of q2. For p2=0, the disk is unstable if q2<0.228, while for q2=0, it is unstable if p2<1. The combined effect of rotation and magnetic field makes the disk more stable than a naive linear extrapolation, that is, the disk with p2+q2/ 0.228=1 is stable and far from the instability region in general. The waves with short wavelength are stabilized by gas pressure while those with long wavelength are stabilized by rotation. For example, for p2=0.25 and q2/ 0.228=0.46, the disk becomes marginally stable if the wavelength is about four times the scale height of the disk.
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