Local Three-Dimensional MHD Simulations of the Parker Instability in Differentially Rotating Disks View Full Text


Ontology type: schema:Chapter     


Chapter Info

DATE

1998

AUTHORS

T. Matsuzaki , R. Matsumoto , T. Tajima , K. Shibata

ABSTRACT

Recently, several authors (Hawley et al. 1995; Matsumoto & Tajima 1995; Brandenburg et al. 1995) have carried out three-dimensional local magnetohydrodynamic (MHD) simulations of magnetized accretion disks. In gravitationally stratified disks, buoyant escape of magnetic flux due to the Parker instability (Parker 1966) may limit the strength of magnetic fields inside the disk. Three-dimensional MHD simulations of weakly magnetized Keplerian disks (Stone et al. 1996), however, showed little signature of the Parker instability. This is because in high-β disks (β = Pgas/Pmag≫ 1), the growth rate of the Parker instability γP ~ 0.2 – 0.5vA/H ~ 0.3–0.7Ω/β1/2 is much smaller than that of the Balbus & Hawley instability γBH ~ 0.1 – 0.7Ω (Balbus & Hawley 1991). Here vA is the Alfvén speed, H is the disk thickness and Ω is the rotational angular speed. Moreover, the Balbus & Hawley instability may cut off the growth of the Parker instability by disrupting the coherence of the azimuthal magnetic field (Stone et al. 1996). More... »

PAGES

321-324

Book

TITLE

Observational Plasma Astrophysics: Five Years of Yohkoh and Beyond

ISBN

978-94-010-6198-8
978-94-011-5220-4

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/978-94-011-5220-4_52

DOI

http://dx.doi.org/10.1007/978-94-011-5220-4_52

DIMENSIONS

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