Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.337.1245l&link_type=abstract
Monthly Notice of the Royal Astronomical Society, Volume 337, Issue 4, pp. 1245-1251.
Astronomy and Astrophysics
Astronomy
4
Accretion, Accretion Discs, Binaries: Close, Stars: Individual: 1Sax 1324.4-6200, Stars: Neutron, X-Rays: Stars
Scientific paper
We present results of a long ASCA observation made on 2000 February 2, of the X-ray pulsar 1SAX 1324.4-6200, in which the pulse period Pspin was found to be 171.245 +/- 0.012 s, and a possible orbital period Porb of 27 +/- 1 h was discovered. Pspin is significantly larger than the pulse period determined from the previous observations with BeppoSAX (1997 August) and ASCA (1994 August), and the three period values spread over a period of 5.5 yr agree well with a linear spin-down of the pulsar. The best-fitting rate of spin-down, , is +5.2063 +/- 0.0005 × 10-9 s s-1, and is +3.04 × 10-11 s-1, or +9.59 × 10-4 yr-1. However, we cannot rule out the possibility that the overall trend is of spin-up, and the observations represent fluctuations of spin-down. The ASCA X-ray spectrum of 1SAX 1324.4-6200 is rather featureless with an upper limit for a narrow iron line at 6.4 keV of 80 eV. The possible nature of the pulsar is discussed, the non-transient nature making it unlikely to be a Be system. It is possible that it is a wind-fed supergiant; however, this would require the overall trend in period evolution to be that of spin-up. If the tentative orbital period is real, the supergiant has to be lobe-filling. In fact, the observational evidence is more consistent with the object being a low-mass X-ray binary (LMXB) pulsar, including both spin and orbital periods, and the 5.5-yr apparent duration of spin-down. In this case, the object would join the small number of LMXB pulsars known.
Bałucinska-Church M.
Church M. J.
Lin Xiao-Biao
Nagase Fumiaki
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