Issue |
A&A
Volume 397, Number 1, January I 2003
|
|
---|---|---|
Page(s) | 249 - 256 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20021477 | |
Published online | 11 December 2002 |
X-ray properties of 4U 1543–624
Observatory, PO Box 14, 00014 University of Helsinki, Finland
Received:
4
July
2002
Accepted:
8
October
2002
4U 1543–624 is a relatively bright persistent low-mass X-ray
binary. Analysis of archival data from ASCA, SAX and RXTE is presented.
The X-ray continuum be can modeled with the standard low-mass X-ray
binary spectrum, an isothermal blackbody and a Comptonized component.
Variations in the luminosity and flux ratio of the continuum components
are seen. An increase in luminosity is accompanied by a decrease
in the blackbody luminosity and a hardening of the spectrum.
Most low-mass X-ray binaries have softer spectra and higher
blackbody luminosities in high luminosity states.
The Fe line is seen only in the high luminosity spectra.
A narrow feature near 0.7 keV, previously detected in the
ASCA data, is also seen in the SAX data.
A qualitative model of the system is presented. The X-ray observations
can be explained by a low inclination system (face-on disk)
containing a slowly (
ms) rotating neutron star.
A slowly rotating neutron star would imply either that the system is a
young low-mass X-ray binary, or that the accretion rate
is unusually low. The empirical relation between optical and X-ray
luminosity and orbital period suggests a relatively short period.
Key words: binaries: close / stars: individual: 4U 1543–624 / X-rays: binaries
© ESO, 2003
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