Other
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987stin...8821882h&link_type=abstract
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Astronomical Spectroscopy, Pulsars, Stellar Spectra, Supernova Remnants, X Ray Binaries, Accretion Disks, Exosat Satellite, Pulse Duration, Stellar Rotation
Scientific paper
The X-ray pulsar, 1E2259+586, and the associated supernova remnant, G109.1-1.0 were observed with the EXOSAT on 1984 December 1/2. The pulse period at this epoch was 6.978720 + or - 0.000006 (1 sigma) s, indicating that between 1981 and 1984 the pulsar was spinning down with an average secular rate of change of the spin period given by P dot/P = +(3.3 + or - 0.2) x 0.000001/yr. The pulse shape is stable on a time-scale of hours and shows energy dependence. Measured P dot is sufficiently small to exclude the possibility that this source is an isolated pulsar powered by rotational energy losses and so the pulsar is probably powered by accretion from a low mass companion. In the context of theories of accretion disk torques, 1E2259+586 is a fast rotator spinning at close to its equilibrium period. Data are not compatible with the 2300 s binary orbital solution reported by Fahlman and Gregory (1983) and analysis shows that the axsin(i) for this system less than or = to 160 lt-msec (3 sigma upper limit). The pulsed spectrum of 1E2259+586 is softer than that of any other known binary X-ray pulsar. Spectral fits indicate a thermal bremsstrahlung temperature of 1 keV or a power law photon index of 3.5.
Coe Malcolm J.
Davies Steven R.
Dennerl Konrad
Hanson C. G.
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