Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/0110670)
· References in the article
· Citations to the Article (25) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
Magnetic activity in accretion disc boundary layers
Authors:
Armitage, Philip J.
Affiliation:
AA(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 330, Issue 4, pp. 895-900. (MNRAS Homepage)
Publication Date:
03/2002
Origin:
MNRAS
Astronomy Keywords:
ACCRETION, ACCRETION DISCS, MAGNETIC FIELDS, MHD, NOVAE, CATACLYSMIC VARIABLES, STARS: PRE-MAIN-SEQUENCE, STARS: WINDS, OUTFLOWS, accretion, accretion discs, magnetic fields, MHD, novae, cataclysmic variables, stars: pre-main-sequence, stars: winds, outflows
DOI:
10.1046/j.1365-8711.2002.05152.x
Bibliographic Code:
2002MNRAS.330..895A

Abstract

We use three-dimensional magnetohydrodynamic simulations to study the structure of the boundary layer between an accretion disc and a non-rotating, unmagnetized star. Under the assumption that cooling is efficient, we obtain a narrow but highly variable transition region in which the radial velocity is only a small fraction of the sound speed. A large fraction of the energy dissipation occurs in high-density gas adjacent to the hydrostatic stellar envelope, and may therefore be reprocessed and largely hidden from view of the observer. As suggested by Pringle, the magnetic field energy in the boundary layer is strongly amplified by shear, and exceeds that in the disc by an order of magnitude. These fields may play a role in generating the magnetic activity, X-ray emission and outflows in disc systems where the accretion rate is high enough to overwhelm the stellar magnetosphere.

Printing Options

Send high resolution image to Level 2 Postscript Printer
Send low resolution image to Level 2 Postscript Printer
Send low resolution image to Level 1 Postscript Printer
Get high resolution PDF image
Get low resolution PDF
Send 300 dpi image to PCL Printer
Send 150 dpi image to PCL Printer

More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints