Pulse phase variations of the X-ray spectral features in the radio-quiet neutron star 1E 1207-5209

Details Pulse phase variations of the X-ray spectral features in the radio-quiet neutron star 1E 1207-5209 Pulse phase variations of the X-ray spectral features in the radio-quiet neutron star 1E 1207-5209

2002-07-14

arxiv.org/abs/astro-ph/0207296v2

Astrophys.J. 581 (2002) 1280-1285

Astronomy and Astrophysics

Astrophysics

6 pages, 3 Postscript figures. Minor changes; accepted for publication in The Astrophysical Journal

Scientific paper

10.1086/344435

We present the results of an XMM-Newton observation of the radio-quiet X-ray pulsar 1E 1207-5209 located at the center of the shell-like supernova remnant G296.5+10.0. The X-ray spectrum is characterized by the presence of two phase-dependent absorption lines at energies ~0.7 keV and ~1.4 keV. Moreover, these broad spectral features have significant substructure, suggesting that they are due to the blending of several narrower lines. We interpret such features as evidence for an atmosphere containing metals and a magnetic field value of a few 10^12 G, consistent with the observed spin-down rate P_dot=(1.98+/-0.83)*10^(-14) s/s. Since 1E 1207-5209 is the only X-ray emitting pulsar showing evidence of such features, we tentatively link them to the unique combination of age and energetics that characterize this object. We suggest that a young age and a low level of magnetospheric activity are favorable conditions for the detection of atomic spectral features from metals in neutron star atmospheres, which would be either blanketed by a thin layer of accreted hydrogen in older objects or masked by non-thermal processes in young energetic pulsars.

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