X-ray Timing of PSR B1509-58

Details X-ray Timing of PSR B1509-58 X-ray Timing of PSR B1509-58

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000head....5.3309r&link_type=abstract

American Astronomical Society, HEAD Meeting #5, #33.09; Bulletin of the American Astronomical Society, Vol. 32, p.1241

Astronomy and Astrophysics

Astronomy

Scientific paper

We have monitored the stable pulsar B1509-58 in the 2-100 keV X-ray band with RXTE since the start of that mission, in January 1996. The X-ray pulse lags the radio pulse by 0.30 +/- 0.01 in phase and there is no indication of this lag's depending on energy. Starting from the radio timing ephemeris, we have derived a single X-ray timing ephemeris that fits the entire monitoring period, using the pulse frequency and its first, second, and third derivatives. This provides a value of 2.85 for the breaking index, in agreement with earlier determinations, but the third derivative is too high to be consistent with a simple spin-down law. Of special interest are the timing residuals which either require a higher order po;ynomial fit or exhibit a (quasi?) periodic behavior with a period of about 710 days and an amplitude of 3 to 4 ms. This work has been supported by NASA grant NAG5-7335.

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