Volume 531, July 2011
|Number of page(s)||7|
|Section||Stellar structure and evolution|
|Published online||01 July 2011|
Secular spin-down of the AMP XTE J1751-305
INAF/Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, 09012 Capoterra, Italy
2 Università di Cagliari, Dipartimento di Fisica, SP Monserrato-Sestu km 0, 7, 09042 Monserrato (CA), Italy
3 Dipartimento di Scienze Fisiche e Astronomiche, Università di Palermo, via Archirafi 36, 90123 Palermo, Italy
4 Osservatorio Astronomico di Roma, Sede di Monteporzio Catone, via Frascati 33, 00040 Roma, Italy
Received: 28 April 2010
Accepted: 6 May 2011
Context. Of the 13 known accreting millisecond pulsars, only a few have displayed more than one outburst during the RXTEera. After its main outburst in 2002, XTE J1751-305 showed an additional three dim outbursts. We report on the timing analysis of the latest one, which occurred on October 8, 2009 and was serendipitously observed from its very beginning by RXTE.
Aims. By detecting the pulsation during more than one outburst, we derive a stronger constraint of the orbital parameters and their evolution, and we can track the secular spin frequency evolution of the source.
Methods. Using the RXTEdata of the last outburst of the AMP XTE J1751-305, we performed a timing analysis to more accurately constrain the orbital parameters. Because of the low quality of the data statistics, we applied an epoch-folding search technique to the whole data set to improve the local estimate of the time of ascending node passage.
Results. Using this new orbital solution, we epoch-folded data obtaining three pulse phase delays over a time span of 1.2 days, that we fitted using a constant spin frequency model. Comparing this barycentric spin frequency with that of the 2002 outburst, we obtained a secular spin frequency derivative of −0.55(12) × 10-14 Hz s-1. We estimate the pulsar’s magnetic dipole value by assuming that the secular spin-down is due to a rotating magneto dipole emission, to be consistent with what is assumed for radio pulsars. We derive an estimate of the magnetic field strength at the polar cap of BPC = 4.0(4) × 108 G, for a neutron star mass of 1.4 M⊙, assuming the Friedman Pandharipande Skyrme equation of state.
Key words: stars: neutron / stars: magnetic field / pulsars: general / pulsars: individual: XTE J1751-305 / X-rays: binaries
© ESO, 2011
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.