Volume 451, Number 1, May III 2006
|Page(s)||267 - 272|
|Section||Stellar structure and evolution|
|Published online||25 April 2006|
Study of the cyclotron feature in MXB 0656-072
School of Physics & Astronomy, University of Southampton, Highfield, SO17 1BJ, UK e-mail: email@example.com
2 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
3 Institut für Astronomie und Astrophysik – Astronomie, Sand 1, 72076 Tübingen, Germany
4 INTEGRAL Science Data Centre, 16 Ch. d'Écogia, 1290 Versoix, Switzerland
5 Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093-0424, USA
6 Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94702-7450, USA
7 European Space Astronomy Centre (ESAC), European Space Agency, PO Box 50727, 28080, Madrid, Spain
Accepted: 26 January 2006
We have monitored a type II outburst of the Be/X-ray binary MXB 0656-072 in a series of pointed RXTE observations during October through December 2003. The source spectrum shows a cyclotron resonance scattering feature at keV, corresponding to a magnetic field strength of G and is stable through the outburst and over the pulsar spin phase. The pulsar, with an average pulse period of s, shows a spin-up of 0.45 s over the duration of the outburst. From optical data, the source distance is estimated to be kpc and this is used to estimate the X-ray luminosity and a theoretical prediction of the pulsar spin-up during the outburst.
Key words: X-rays: stars / stars: magnetic fields / stars: pulsars: individual: MXB 0656-072
© ESO, 2006
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