Publications (3)0 Total impact
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Article: Diagnostics of very early stages of the classical nova explosion by the modeling of its X-ray emission
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ABSTRACT: We present a spherically symmetric model of the interaction of classical nova ejecta with the matter of the companion star stellar wind. We compare its predictions with the data of observations of the unusual bright X-ray transient CI Cam and demonstrate that the outburst in 1998 can be explained as the X-ray emission at early stages of the classical nova explosion in the binary system. The X-ray outburst was observed almost immediately after the start of the motion of the ejecta (within 0.1-0.5 days) which give us the possibility to constrain two parameters of the explosions - the velocity and the mass of the ejecta. We show that the ejecta velocity was ~2700 km/s and remained at this value over ~2 day after the beginning of the explosion, that indicates the presence of the external forces acting on the ejecta. The mass of the ejecta was ~ 10-7 - 10-6M.Journal of Physics Conference Series 07/2009; 172(1):012045. -
Article: Diagnostics of the black hole candidate SS433 with the RXTE
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ABSTRACT: 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, if the X-ray opaque size of the star is not larger than 1.2R_{Roche, secondary}.10/2006; -
Article: Diagnostics of SS433 with the RXTE
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ABSTRACT: We present analysis of 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 a strong photoabsorption near the optical star, probably due to its powerful dense wind. Assuming that a precessing accretion disk is thick, we recover the temperature profile in the X-ray emitting jet that best fits the observed precessional variations of the X-ray emission temperature. The hottest visible part of the X-ray jet is located at a distance of $l_0/a\sim0.06-0.09$, or $\sim2-3\times10^{11}$cm from the central compact object and has a temperature of about $T_{\rm max}\sim30$ 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 put a lower limit on the size of the optical component $R/a\ga0.5$ and an upper limit on a mass ratio of binary companions $q=M_{\rm x}/M_{\rm opt}\la0.3-0.35$. The size of the eclipsing region can be larger than secondary's Roche lobe because of substantial photoabsorption by dense stellar wind. This must be taken into account when evaluating the mass ratio from analysis of X-ray eclipses.08/2006;
