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/0208527)
· References in the article
· Citations to the Article (21) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (3)
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
The origin of the rebrightening in soft X-ray transient outbursts
Authors:
Truss, M. R.; Wynn, G. A.; Murray, J. R.; King, A. R.
Affiliation:
AA(Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH), AB(Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH), AC(Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH), AD(Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH)
Publication:
Monthly Notice of the Royal Astronomical Society, Volume 337, Issue 4, pp. 1329-1339. (MNRAS Homepage)
Publication Date:
12/2002
Origin:
MNRAS
Astronomy Keywords:
accretion, accretion discs, instabilities, methods: numerical, binaries: close, stars: individual: A0620-003, X-rays: stars
DOI:
10.1046/j.1365-8711.2002.05986.x
Bibliographic Code:
2002MNRAS.337.1329T

Abstract

We present a model of an outburst of the soft X-ray transient A0620-003. A two-dimensional time-dependent smoothed particle hydrodynamics scheme is used to simulate the evolution of the accretion disc through a complete outburst. The scheme includes the full tidal potential of the binary and a simple treatment of the thermal-viscous disc instability. In the case where the mass accretion rate on to the primary determines the fraction of the disc that can be kept in a hot, high-viscosity state by the resulting X-ray emission, we find that the shape of the X-ray light curve is ultimately determined by the relative sizes of the irradiated and unirradiated parts of the disc and the growth time-scale of the tidal instability. The model accounts for the rebrightening that has been observed in the light curves of A0620-003 and several other transients. The primary maximum and subsequent decline are caused by the accretion of gas within the irradiated portion of the disc, while the secondary maximum is caused by the accretion of gas in the outer part of the disc, which is initially shadowed from the central X-rays, but subject to tidal forces. We propose that tidal effects at the disc edge can be sufficient to drive accretion on a time-scale shorter than that expected for a standard alpha-viscosity disc. The final decay is subsequently controlled by the gradual retreat of the irradiated portion of the disc. If the entire disc is kept in the high-viscosity state by the irradiation, no rebrightening is possible.

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