Diagnostics of SS433 with the RXTEстатья

Статья опубликована в высокорейтинговом журнале

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Дата последнего поиска статьи во внешних источниках: 18 июля 2013 г.

Работа с статьей

[1] Diagnostics of ss433 with the rxte / E. Filippova, M. Revnivtsev, S. Fabrika et al. // Astronomy and Astrophysics. — 2006. — Vol. 460, no. 1. — P. 125–131. We present our analysis of the extensive monitoring of SS433 by the RXTE observatory collected over the period 1996-2005. The difference between energy spectra taken at different precessional and orbital phases shows the presence of strong photoabsorption (N_H>1023 1/cm2) near the optical star, probably due to its powerful, dense wind. Therefore the size of the secondary deduced from analysis of X-ray orbital eclipses might be significantly larger than its Roche lobe size, which must be taken into account when evaluating the mass ratio from analysis of X-ray eclipses. Assuming that a precessing accretion disk is geometrically thick, we recover the temperature profile in the X-ray emitting jet that best fits the observed precessional variations in the X-ray emission temperature. The hottest visible part of the X-ray jet is located at a distance of l_0/a∼0.06-0.09, or (2-3)×1011 cm from the central compact object, and has a temperature of about T_max∼30 keV. We discovered appreciable orbital X-ray eclipses at the crossover precessional phases (jets are in the plane of the sky, disk is edge-on), which under model assumptions put a lower limit on the size of the optical component R/a⪆0.5 and an upper limit on a mass ratio of binary companions q=M_x/M_opt<=0.3-0.35, if the X-ray opaque size of the star is not larger than 1.2R_Roche, secondary. [ DOI ]

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