Origin of Large and Highly Variable Changes in the Apparent Spin Frequencies of Accretion-Powered Millisecond Pulsars

Details Origin of Large and Highly Variable Changes in the Apparent Spin Frequencies of Accretion-Powered Millisecond Pulsars Origin of Large and Highly Variable Changes in the Apparent Spin Frequencies of Accretion-Powered Millisecond Pulsars

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0407l&link_type=abstract

American Astronomical Society, HEAD meeting #9, #4.07; Bulletin of the American Astronomical Society, Vol. 38, p.347

Astronomy and Astrophysics

Astronomy

Scientific paper

The spin-frequency behavior of accretion-powered millisecond pulsars is usually inferred by power spectral analysis of their X-ray waveforms. The reported behavior of the spin frequencies of several accretion-powered millisecond pulsars is puzzling in two respects. First, analysis of the waveforms of these pulsars indicates that their spin frequencies are changing faster than predicted by the standard model of accretion torques. Second, there are wild swings of both signs in their apparent spin frequencies that are not correlated with the mass accretion rates inferred from their X-ray fluxes. We have computed the expected X-ray waveforms of pulsars like these, including special and general relativistic effects, and find that the changes in their waveforms produced by physically plausible changes in the flow of accreting matter onto their surfaces can explain their apparently anomalous spin-frequency behavior. This research was supported in part by NASA grant NAG 5-12030, NSF grant AST 0098399, and funds of the Fortner Endowed Chair at Illinois, and NSF grant AST 0098436 at Maryland.

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