Diagnostics of the black hole candidate SS433 with the RXTE

Diagnostics of the black hole candidate SS433 with the RXTE

Authors: E. Filippova (1,2), M. Revnivtsev (1,2), S. Fabrika (3), K. Postnov (4), E. Seifina (4) ((1) MPA, Garching, Germany,(2) IKI, Moscow, Russia, (3) SAO, Nizhnij Arkhyz, Russia,(4) SAI, Moscow, Russia)
Comments: 9 pages, 9 figures, accepted for publication in Astronomy and Astrophysics

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>10^{23}cm^{-2}) 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*10^{11}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,>

Full-text: PostScript, PDF, or Other formats

译文：

跟进动有关，似乎比较好上手!