Journal Article

Kelvin–Helmholtz instability at the interface of a disc–corona system

Mohsen Shadmehri and Perikles Rammos

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 406, issue 4, pages 2627-2632
Published in print August 2010 | ISSN: 0035-8711
Published online August 2010 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2010.16861.x
Kelvin–Helmholtz instability at the interface of a disc–corona system

Show Summary Details

Preview

We study Kelvin–Helmholtz (KH) instability at the interface of a disc and corona system by doing a linear perturbation analysis. The disc is assumed to be thin; however, the corona is considered to be nearly quasi-spherical because of its high temperature. Under these circumstances, the interface is subject to the KH instability for a given set of the input parameters. Growth rates of the KH unstable modes are calculated for a wide range of the input parameters. We show that for a certain range of the perturbations, the unstable KH perturbations are growing with time-scales comparable to the inverse of the angular velocity of the accretion disc (dynamical time-scale). Thus, KH instability at the interface of a disc–corona may have enough time to affect the dynamical structure of its underlying accretion disc by possible exchange of the mass, angular momentum or even energy. Our linear analysis shows that KH instability may provide a mechanism for such exchanges between a disc and its corona.

Keywords: accretion, accretion discs; black hole physics; galaxies: active

Journal Article.  3099 words.  Illustrated.

Subjects: Astronomy and Astrophysics

Full text: subscription required

How to subscribe Recommend to my Librarian

Users without a subscription are not able to see the full content. Please, subscribe or login to access all content.