ROSAT observations of pulsed soft X-ray emission from PSR 1055-52

Details ROSAT observations of pulsed soft X-ray emission from PSR 1055-52 ROSAT observations of pulsed soft X-ray emission from PSR 1055-52

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...413l..31o&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 413, no. 1, p. L31-L34.

Astronomy and Astrophysics

Astrophysics

88

Emission Spectra, Pulsars, Rosat Mission, X Ray Spectra, Black Body Radiation, Neutron Stars, Spectral Energy Distribution, X Ray Stars

Scientific paper

Utilizing the position-sensitive proportional counter and the high-resolution imager aboard the orbiting X-ray observatory ROSAT, we have detected pulsations at the radio period from the pulsar PSR 1055-52. The pulse shapes are energy-dependent and show a transition at about 0.5 keV where the phase angle of the pulse peak changes by about -120 deg and the pulsed fraction increases from 11 percent to 63 percent toward larger energies. Simple spectral models are found to be unsatisfactory, while multicomponent models, such as a soft blackbody and hard power-law tail, yield better fits to the pulse-height data. The hard power-law tail is consistent with the extension of the recently reported EGRET results and may indicate a common emission mechanism for the X-ray through GeV gamma-ray regime. The soft blackbody component with T(infinity) = (7.5 +/- 0.6) x 10 exp 5 K, if interpreted as the initial cooling of a neutron star, is consistent with standard cooling models and does not require the presence of exotic components.

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