Timing models for the long-orbital period binary pulsar PSR B1259-63

Details Timing models for the long-orbital period binary pulsar PSR B1259-63 Timing models for the long-orbital period binary pulsar PSR B1259-63

1998-03-16

arxiv.org/abs/astro-ph/9803182v1

Astronomy and Astrophysics

Astrophysics

LaTeX, 9 pages, 8 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.1998.01700.x

The pulsar PSR B1259-63 is in a highly eccentric 3.4-yr orbit with the Be star SS 2883. Timing observations of this pulsar, made over a 7-yr period using the Parkes 64-m radio telescope, cover two periastron passages, in 1990 August and 1994 January. The timing data cannot be fitted by the normal pulsar and Keplerian binary parameters. A timing solution including a (non-precessing) Keplerian orbit and timing noise (represented as a polynomial of fifth order in time) provide a satisfactory fit to the data. However, because the Be star probably has a significant quadrupole moment, we prefer to interpret the data by a combination of timing noise, dominated by a cubic phase term, and $\dot\omega$ and $\dot x$ terms. We show that the $\dot\omega$ and $\dot x$ are likely to be a result of a precessing orbit caused by the quadrupole moment of the tilted companion star. We further rule out a number of possible physical effects which could contribute to the timing data of PSR B1259-63 on a measurable level.

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