ELECTROMAGNETIC STREAMING INSTABILITIES OF MAGNETIZED ACCRETION DISKS WITH STRONG COLLISIONAL COUPLING OF SPECIES

Journal Article · Fri Apr 10 04:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/695/1/46; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21296274

Electromagnetic streaming instabilities of multicomponent collisional magnetized accretion disks are studied. Sufficiently ionized regions of the disk are explored where there is strong collisional coupling of neutral atoms with both ions and dust grains simultaneously. The steady state is investigated in detail and the azimuthal and radial background velocities of species are calculated. The azimuthal velocity of ions, dust grains, and neutrals is found to be less than the Keplerian velocity. The radial velocity of neutrals and dust grains is shown to be directed inward of the disk. The general solution for the perturbed velocities of species taking into account collisions and thermal pressure is obtained. The effect on the collisional frequencies, due to density perturbations of charged species and neutrals, is included. It is shown that dust grains can be involved in the fast electromagnetic perturbations induced by the ions and electrons through the strong collisions of these grains with neutrals that in turn have a strong collisional coupling with the ions. The dispersion relation for the vertical perturbations is derived and its unstable solutions due to different background velocities of ions and electrons are found. The growth rates of the streaming instabilities considered can be much larger than the Keplerian frequency.

• OSTI ID: 21296274
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 695; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

99 GENERAL AND MISCELLANEOUS
ACCRETION DISKS
DISPERSION RELATIONS
INSTABILITY
MAGNETIC FIELDS
PERTURBATION THEORY
PLASMA WAVES
RADIAL VELOCITY
STEADY-STATE CONDITIONS