Observations of Magnetic Fields in Accreting Pulsars with the RXTE

Details Observations of Magnetic Fields in Accreting Pulsars with the RXTE Observations of Magnetic Fields in Accreting Pulsars with the RXTE

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprx11002c&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Using a consistent set of models, we parameterized the X--Ray spectra of all accreting pulsars in the phRossi X--Ray Timing Explorer (RXTE) database that exhibit ``cyclotron lines.'' Cyclotron lines are line-like spectral features that arise from resonant scattering of photons on electrons, and whose energies are directly proportional to the neutron star B-field. The sources in our sample are Her X-1, 4U 0115+63, Cen X-3, 4U 1626-67, XTE J1946-274, Vela X-1, 4U 1907+09, 4U 1538-52, GX 301-2, and X Per. We searched for correlations among the spectral parameters, concentrating on how the cyclotron line energy related to the continuum and therefore how the neutron star B-field influenced the X-Ray emission. As expected we found a correlation between the cyclotron energy and the spectral cutoff energy. However, with our consistent set of fits we found that the relationship is more complex than what has been reported previously. Also, we found that not only does the width of the cyclotron line correlate with the energy (as suggested by theory), but the relative width correlates with the depth of the feature. We discuss the implications of these results.

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