Evidence for a Millisecond Pulsar in 4U 1636-53 During a Superburst

Details Evidence for a Millisecond Pulsar in 4U 1636-53 During a Superburst Evidence for a Millisecond Pulsar in 4U 1636-53 During a Superburst

2002-05-24

arxiv.org/abs/astro-ph/0205435v1

Astrophys.J.577:337-345,2002

Astronomy and Astrophysics

Astrophysics

27 pages, 9 figures, AASTeX, accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/342152

We report the discovery with the Proportional Counter Array on board the Rossi X-ray Timing Explorer of highly coherent 582 Hz pulsations during the February 22, 2001 (UT) ``superburst'' from 4U 1636-53. The pulsations are detected during an 800 s interval spanning the flux maximum of the burst. Within this interval the barycentric oscillation frequency increases in a monotonic fashion from 581.89 to 581.93 Hz. The predicted orbital motion of the neutron star during this interval is consistent with such an increase as long as optical maximum corresponds roughly with superior conjunction of V801 Arae, the optical companion to the neutron star in 4U 1636-53. We show that a range of circular orbits with velocity 90 < v sin i < 175 km/s and fractional phase 0.336 > p > 0.277 for the neutron star can provide an excellent description of the frequency and phase evolution. The average pulse profile is sinusoidal and the time averaged pulsation amplitude, as inferred from the half amplitude of the sinusoid is 1%, smaller than typical for burst oscillations observed in normal thermonuclear bursts. We do not detect any higher harmonics nor the putative subharmonic near 290 Hz. The 90% upper limits on signal amplitude at the subharmonic and first harmonic are 0.1% and 0.06%, respectively. The coherent pulsation provides compelling evidence for a rapidly rotating neutron star in 4U 1636-53, and further supports the connection of burst oscillation frequencies with the spin frequencies of neutron stars. Our results provide further evidence that some millisecond pulsars are spun up via accretion in LMXBs. We also discuss the implications of our orbital velocity constraint for the masses of the components of 4U 1636-53.

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