Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic On-line Article (HTML)
· arXiv e-print (arXiv:0810.4915)
· On-line Data
· Table of Contents
· References in the Article
· Citations to the Article (2) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Properties of X-ray binaries in the Magellanic Clouds from RXTE and Chandra observations
Authors:
Corbet, R. H. D.; Coe, M. J.; McGowan, K. E.; Schurch, M. P. E.; Townsend, L. J.; Galache, J. L.; Marshall, F. E.
Affiliation:
AA(University of Maryland, Baltimore County/CRESST, 1000 Hilltop Circle, Baltimore, MD 21250, USA; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AB(School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK), AC(School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK), AD(School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK), AE(School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AG(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA)
Publication:
The Magellanic System: Stars, Gas, and Galaxies, Proceedings of the International Astronomical Union, IAU Symposium, Volume 256, p. 361-366
Publication Date:
03/2009
Origin:
CUP
Keywords:
stars: emission-line, Be, stars: neutron, pulsars: general, Magellanic Clouds, X-rays: binaries
DOI:
10.1017/S1743921308028718
Bibliographic Code:
2009IAUS..256..361C

Abstract

The X-ray binary population of the SMC is very different from that of the Milky Way consisting, with one exception, entirely of transient pulsating Be/neutron star binaries. We have now been monitoring these SMC X-ray pulsars for over 10 years using the Rossi X-ray Timing Explorer with observations typically every week. The RXTE observations have been complemented with surveys made using the Chandra observatory. The RXTE observations are non-imaging but enable detailed studies of pulsing sources. In contrast, Chandra observations can provide precise source locations and detections of sources at lower flux levels, but do not provide the same timing information or the extended duration light curves that RXTE observations do. We summarize the results of these monitoring programs which provide insights into both the differences between the SMC and the Milky Way, and the details of the accretion processes in X-ray pulsars.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

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