Volume 556, August 2013
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||19 July 2013|
XMM-Newton and Swift observations of XTE J1743-363⋆
ISDC Data Centre for Astrophysics, department of Astronomy, University of
Geneva, Chemin d’Écogia
2 INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, 90146 Palermo, Italy
3 INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate ( LC), Italy
4 International Space Science Institute (ISSI) Hallerstrasse 6, 3012 Bern, Switzerland
5 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00044 Roma, Italy
Accepted: 6 June 2013
XTE J1743-363 is a poorly known hard X-ray transient, which displays short and intense flares similar to those observed from supergiant fast X-ray transients. The probable optical counterpart shows spectral properties similar to those of an M8 III giant, thus suggesting that XTE J1743-363 belongs to the class of the symbiotic X-ray binaries class. In this paper we report on the first dedicated monitoring campaign of the source in the soft X-ray range with XMM-Newton and Swift /XRT. These observations confirmed the association of XTE J1743-363 with the previously suggested M8 III giant and the classification of the source as a member of the symbiotic X-ray binaries. In the soft X-ray domain, XTE J1743-363 displays a high absorption (~6 × 1022 cm-2) and variability on time scales of hundreds to few thousand seconds, typical of wind-accreting systems. A relatively faint flare (peak X-ray flux 3 × 10-11 erg/cm2/s) lasting ~4 ks is recorded during the XMM-Newton observation and interpreted in terms of the wind accretion scenario.
Key words: X-rays: binaries / X-rays: individuals: XTE J1743-363
Table 2 is available in electronic for at http://www.aanda.org
© ESO, 2013
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