Volume 474, Number 1, October IV 2007
|Page(s)||137 - 143|
|Section||Stellar structure and evolution|
|Published online||13 August 2007|
XMM-Newton observation of the persistent Be/neutron star system X Persei at a high-luminosity level
INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milano, Italy e-mail: email@example.com
Accepted: 8 July 2007
We report on the XMM-Newton observation of the HMXRB X Persei, the prototype of the persistent and low-luminosity Be/neutron star pulsars, which was performed in February 2003. The source was detected at a luminosity level of ~1.41035 erg s-1, which is the highest level of the latest three decades. The pulsation period has increased to 839.3 s, thus confirming the overall spin-down of the neutron star detected in the previous observations. The folded light-curve has a complex structure, with features not observed at lower luminosities, and shows a significant energy dependence. The spectral analysis reveals the presence of a significant excess, at low energies, over the main power-law spectral component, which can be described by a black-body spectrum of high temperature ( 1.5 keV) and small emitting region ( 360 m); its properties are consistent with a polar-cap origin. Phase-resolved spectroscopy shows that the emission spectrum varies along the pulse period, but it is not possible to prove whether the thermal component is pulsed or not.
Key words: X-rays: binaries / accretion, accretion disks / stars: emission-line, Be / stars: pulsars: individual: X Persei / X-rays: individuals: 4U 0352+309
© ESO, 2007
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