Spectra and pulse period of the binary X-ray pulsar 4U 1538-52

Details Spectra and pulse period of the binary X-ray pulsar 4U 1538-52 Spectra and pulse period of the binary X-ray pulsar 4U 1538-52

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...314..619m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 314, March 15, 1987, p. 619-628.

Astronomy and Astrophysics

Astronomy

29

Binary Stars, Neutron Stars, Pulsars, X Ray Binaries, K Lines, Line Spectra, Metallicity, Milky Way Galaxy, Stellar Evolution

Scientific paper

The 530 s binary X-ray pulsar 4U 1538-52 was observed from the X-ray astronomy satellite Tenma in 1983 June-July. An improved orbital ephemeris was derived. Also, high-quality X-ray spectra were obtained by taking into account the contribution of the Galactic ridge emission. It was found that the iron K-line emission from this source is weak, contrary to previous reports. The observed pulsation period, about 529.8 s, is about 0.4 s longer than that measured in 1976-1977, implying an average spin-down rate of 3.8 x 10 to the -9th s/s. In addition, there is some evidence for a much larger rate of instantaneous period increase. These results suggest that 4U 1538-52 is a wind-fed pulsar, and its pulsation period changes in a random-walk manner in response to fluctuations in the external torque. This is very similar to the case of Vela X-1.

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