Abstract
| Lingua originale | English |
|---|---|
| pagine (da-a) | - |
| Numero di pagine | 7 |
| Rivista | ASTRONOMY & ASTROPHYSICS |
| Volume | 530 |
| Stato di pubblicazione | Published - 2011 |
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All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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X-ray spectroscopy of MXB 1728-34 with XMM-Newton. / Di Salvo, Tiziana; Iaria, Rosario; Burderi; Wilms, Jörn; Papitto; Riggio; Barragán; Dauser; Egron.
In: ASTRONOMY & ASTROPHYSICS, Vol. 530, 2011, pag. -.Risultato della ricerca: Article
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TY - JOUR
T1 - X-ray spectroscopy of MXB 1728-34 with XMM-Newton
AU - Di Salvo, Tiziana
AU - Iaria, Rosario
AU - Burderi, null
AU - Wilms, Jörn
AU - Papitto, null
AU - Riggio, null
AU - Barragán, null
AU - Dauser, null
AU - Egron, null
PY - 2011
Y1 - 2011
N2 - We analyzed 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 × 1036 d5.1 kpc2 erg s-1. 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° < i < 60°.
AB - We analyzed 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 × 1036 d5.1 kpc2 erg s-1. 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° < i < 60°.
KW - line: formation, line: identification, stars: neutron, stars: individual: MXB 1728, 34, X-rays: binaries, X-rays: general
UR - http://hdl.handle.net/10447/61884
UR - http://adsabs.harvard.edu/abs/2011A%26A...530A..99E
M3 - Article
VL - 530
SP - -
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
ER -