Internal Gravity Wave in Accretion Disks and its Coupling with Magnetorotational Instability

Details Internal Gravity Wave in Accretion Disks and its Coupling with Magnetorotational Instability Internal Gravity Wave in Accretion Disks and its Coupling with Magnetorotational Instability

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.7104n&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #71.04; Bulletin of the American Astronomical Society, Vol. 34, p.760

Astronomy and Astrophysics

Astronomy

Scientific paper

We study the stability of the internal gravity wave(IGW) in accretion disks. The IGW can excite in a disk because of its vertical stratification. Quite different from the case without shear, the IGW is destabilized by the flow shear, which also localizes the eigenmode in the radial direction. Our eigenmode analysis shows that the growth rate in pure hydrodynamical disk is quite small[Im(ω )/Ω =O(0.01)], where Ω is the rotational period. Despite the small growth rate in pure hydrodynamical disks, the coupling of the IGW with the magnetorotational instability(MRI) allow the unstable IGW mode to have larger growth rate[Im(ω )/Ω =O(0.1)] in the weak magnetic field regime(ω A/Ω <0.1), accelerating the evolution of disks. As magnetic field grows by the MRI(ω A/Ω >0.1), the MRI will take over the IGW instability and becomes a dominant instability. As a conclusion, we sugget a new scenario for pure hydrodynamical disks and in weakly magnetized disks such as galactic and quasar disks, as well as stellar and protoplanetary disks. Unstable IGW mode and its coupling with MRI accelarate the evolution of accretion disks faster than the pure MRI, and the Parker instability can be turned on by the excited IGW mode in later stage, accelerating the structure and star formation in accretion disks.

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