Volume 520, September-October 2010
|Number of page(s)||4|
|Section||Stellar structure and evolution|
|Published online||23 September 2010|
INTEGRAL/IBIS observations of a hard X-ray outburst in high-mass X-ray binary 4U 2206+54
National Astronomical Observatories, Chinese Academy of
Sciences, Beijing 100012, PR China e-mail: firstname.lastname@example.org
Accepted: 20 July 2010
Aims. 4U 2206+54 is a wind-fed high-mass X-ray binary with a main-sequence donor star. The nature of its compact object has been recently identified as a slow-pulsation magnetized neutron star.
Methods. INTEGRAL/IBIS observations have a long-term hard X-ray monitoring of 4U 2206+54 and detected a hard X-ray outburst around 15 December 2005 combined with the RXTE/ASM data.
Results. The hard X-ray outburst had a double-flare feature with a duration of ~2 days. The first flare showed a fast rise and long-term decaying light curve about 15 h with a peak luminosity of ~4 × 1036 erg s-1 from 1.5–12 keV and a hard spectrum (only significantly seen above 5 keV). The second one had the mean hard X-ray luminosity of 1.3 × 1036 erg s-1 from 20–150 keV with a modulation period at ~5550 s which is the pulse period of the neutron star in 4U 2206+54. Its hard X-ray spectrum from 20–300 keV can be fitted by a broken power-law model with the photon indexes Γ1 ~ 2.3, and Γ2 ~ 3.3, and the break energy is Eb ~ 31 keV or by a bremsstrahlung model of kT ~ 23 keV.
Conclusions. We suggest that the hard X-ray flare could be induced by suddenly enhanced accreting dense materials from stellar winds hitting the polar cap region of the neutron star. This hard X-ray outburst may be a link to supergiant fast X-ray transients though 4U 2206+54 has a different type of companion.
Key words: stars: individual: 4U 2206+54 / stars: neutron / X-rays: binaries / X-rays: bursts
© ESO, 2010
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