Search for Thermal Afterglow from PSR 0656+14

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Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...475..300a&link_type=abstract

Astrophysical Journal v.475, p.300

Astronomy and Astrophysics

Astronomy

3

Stars: Pulsars: Individual Alphanumeric: Psr 0656+14, Stars: Neutron, X-Rays: Stars

Scientific paper

Thermal afterglow caused by transient energy releases in neutron stars could alter the X-ray pulse shape of pulsars by heating a portion of the crust so that more thermal X-rays are emitted at a particular phase. We developed a method to look for such changes in X-ray pulsars. We put a typical lower limit of 3.9 x 1031 ergs s-1 (1.4 x 1035 ergs in a 1 hr exposure) on the average excess X-ray luminosity required to see thermal afterglow from ROSAT data of PSR 0656+14 consisting of three separate observations lasting 3--5 hr. The lower limit obtained allows us to constrain the glitch parameters and the equation of state for neutron stars. In particular, a differentiation could be made between the vortex unpinning model and the starquake model for pulsar glitches if a search for thermal afterglow were performed contemporaneously with glitch observations.

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