XMM-Newton Observation of the High Magnetic Field Radio Pulsar PSR B0154+61

Details XMM-Newton Observation of the High Magnetic Field Radio Pulsar PSR B0154+61 XMM-Newton Observation of the High Magnetic Field Radio Pulsar PSR B0154+61

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.0817g&link_type=abstract

American Astronomical Society, HEAD meeting #8, #08.17; Bulletin of the American Astronomical Society, Vol. 36, p.919

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results from a deep X-ray observation of the radio pulsar B0154+61 performed with the \textit{XMM-Newton} satellite. The pulsar has a characteristic age of 197 kyr, a rotation period of 2.3 seconds and an inferred dipole surface magnetic field strength of 2.1×1013 G, some of the highest values in the radio pulsar population. Our analysis shows that no X-ray emission is detected from the position of B0154+61 with \textit{XMM-Newton}. Using a blackbody model, the derived upper limits on the pulsar's temperature and luminosity are <73 eV and <1.4×1032 ergs s-1, respectively (assuming a distance of 1.7 kpc and a column density NH<3×1021 cm-2). When compared to the values predicted by neutron star cooling models, the above limits are found to favor those requiring rapid cooling, especially when corrections for the presence of a light-element atmosphere and relatively high magnetic field on the neutron star are made. However, the uncertainties in distance, column density and atmospheric composition prevent a definite conclusion. In addition, the limits on the temperature and luminosity of B0154+61 are found to be much lower than those exhibited by the "anomalous X-ray pulsars" (AXPs), although their spin characteristics are comparable, thus leaving unanswered the question of a radio pulsar/AXP connection.

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