X-ray Spectroscopy of MXB 1728-34 with XMM-Newton

Дата и время публикации : 2011-04-04T13:38:23Z

Авторы публикации и институты :
Elise Egron (Università di Cagliari)
Tiziana Di Salvo (Università di Palermo)
Luciano Burderi (Università di Cagliari)
Alessandro Papitto (Università di Cagliari)
Laura Barragán (Dr. Karl Remeis-Sternwarte, Bamberg, and Erlangen Centre for Astroparticle Physics)
Thomas Dauser (Dr. Karl Remeis-Sternwarte, Bamberg, and Erlangen Centre for Astroparticle Physics)
Joern Wilms (Dr. Karl Remeis-Sternwarte, Bamberg, and Erlangen Centre for Astroparticle Physics)
Antonino D’Aì (Università di Palermo)
Alessandro Riggio (Università di Cagliari, INAF – Osservatorio Astronomico di Cagliari)
Rosario Iaria (Università di Palermo)
Natale Renato Robba (Università di Palermo)

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 7 pages, 3 figures, Accepted by A&A on 29.03.2011
Первичная категория: astro-ph.HE

Все категории : astro-ph.HE

Краткий обзор статьи: We have analysed an XMM-Newton observation of the low mass X-ray binary and atoll source MXB 1728-34. The source was in a low luminosity state during the XMM-Newton observation, corresponding to a bolometric X-ray luminosity of 5*10E36 d^2 erg/s, where d is the distance in units of 5.1 kpc. The 1-11 keV X-ray spectrum of the source, obtained combining data from all the five instruments on-board XMM-Newton, is well fitted by a Comptonized continuum. Evident residuals are present at 6-7 keV which are ascribed to the presence of a broad iron emission line. This feature can be equally well fitted by a relativistically smeared line or by a self-consistent, relativistically smeared, reflection model. Under the hypothesis that the iron line is produced by reflection from the inner accretion disk, we can infer important information on the physical parameters of the system, such as the inner disk radius, Rin = 25-100 km, and the inclination of the system, 44{deg} < i < 60{deg}.

Category: Physics