An Explanation for the Properties of the Millisecond X-ray Oscillations Detected in Neutron Stars in LMXBs and the Rarity of These Detections

Details An Explanation for the Properties of the Millisecond X-ray Oscillations Detected in Neutron Stars in LMXBs and the Rarity of These Detections An Explanation for the Properties of the Millisecond X-ray Oscillations Detected in Neutron Stars in LMXBs and the Rarity of These Detections

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.4405l&link_type=abstract

American Astronomical Society, HEAD meeting #12, #44.05

Astronomy and Astrophysics

Astronomy

Scientific paper

Using RXTE, accretion-powered millisecond X-ray oscillations have been detected in 13 of about 130 neutron stars in LMXBs. Three such stars produce detectable oscillations only intermittently. We show that the properties of these oscillations, including their typically small amplitudes, nearly sinusoidal waveforms, and the large, rapid, and correlated variations in the amplitudes and phases of the fundamental and first overtone components of their pulse profiles can be explained if the emitting regions of these stars are typically close to their spin axes and move in response to changes in the accretion flow. We show that this nearly-aligned moving spot model can also explain the absence of detected oscillations in most neutron-star LMXBs and the intermittent detection of oscillations in a few, if the emitting regions of most of these stars are even closer to their spin axes.
These results are based on research supported by NSF grant AST0709015 and the Fortner Chair at Illinois and by NSF grant AST0708424 at Maryland.

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