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Dodin A. V. Potanin S. A. Shatsky N. I. Belinski A. A. Atapin K. E. Burlak M. A. Egorov O. V. Tatarnikov A. M. Postnov K. A. Belvedersky M. I. Burenin R. A. Gilfanov M. R. Medvedev P. S. Meshcheryakov A. V. Sazonov S. Yu. Khorunzhev G. A. Sunyaev R. A. 《Astronomy Letters》2020,46(7):429-438
Astronomy Letters - Based on observations with the new transient double-beam spectrograph (TDS) at the 2.5-m telescope of the Caucasus Mountain Observatory of SAI MSU, we have determined the types... 相似文献
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We describe a model of spectral energy distribution in supercritical accretion disks (SCAD) based on the conception by Shakura and Sunyaev. We apply this model to five ultra-luminous X-ray sources (ULXs). In this approach, the disk becomes thick at distances to the center less than the spherization radius, and the temperature dependence is T ∝ r ?1/2. In this region the disk luminosity is L bol ～ L Edd $\ln \left( {{{\dot M} \mathord{\left/ {\vphantom {{\dot M} {\dot M_{Edd} }}} \right. \kern-0em} {\dot M_{Edd} }}} \right)$ , and strong wind arises forming a wind funnel above the disk. Outside the spherization radius, the disk is thin and its total luminosity is Eddington, L Edd. The thin disk heats the wind from below. From the inner side of the funnel the wind is heated by the supercritical disk. In this paper we do not consider Comptonization in the inner hot winds which must cover the deep supercritical disk regions. Our model is technically similar to the DISKIR model of Gierlinski et al. The models differ in disk type (standard—supercritical) and irradiation (disk—wind).We propose to distinguish between these two models in the X-ray region of about 0.3–1 keV, where the SCAD model has a flat νF ν spectrum, and the DISKIR model never has a flat part, as it is based on the standard α-disk. An important difference between the models can be found in their resulting black hole masses. In application to the ULX spectra, the DISKIR model yields black hole masses of a few hundred solar masses, whereas the SCAD model produces stellar-mass (about 10M⊙) black holes. 相似文献
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Dodin A. V. Shatsky N. I. Belinski A. A. Atapin K. E. Burlak M. A. Zheltoukhov S. G. Tatarnikov A. M. Postnov K. A. Cherepashchuk A. M. Belvedersky M. I. Borisov V. D. Burenin R. A. Gilfanov M. R. Krivonos R. A. Medvedev P. S. Meshcheryakov A. V. Sazonov S. Yu. Sunyaev R. A. Khorunzhev G. A. 《Astronomy Letters》2021,47(10):661-673
Astronomy Letters - Based on observations with the transient double-beam spectrograph (TDS) at the 2.5-m telescope of the Caucasus Mountain Observatory of SAI MSU, we have determined the redshifts... 相似文献
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We study the X-ray variability of SS 433 based on data from the ASCA observatory and the MAXI and RXTE/ASM monitoring missions. Based on the ASCA data, we have constructed the power spectrum of SS 433 in the frequency range from 10?6 to 0.1 Hz, which confirms the presence of a flat portion in the spectrum at frequencies 3 × 10?5?10?3 Hz. The periodic variability (precession, nutation, eclipses) begins to dominate significantly over the stochastic variability at lower frequencies, which does not allow the stochastic variability to be studied reliably. The model in which the flat portion extends to 9.5 × 10?6 Hz, while a power-law rise with an index of 2.6 occurs below provides the best agreement with the observations. The nutational oscillations of the jets with a period of about three days suggests that the time for the passage of material through the disk is less than this value. At frequencies below 4 × 10?6 Hz, the shape of the power spectrum probably does not reflect the disk structure but is determined by external factors, for example, by a change in the amount of material supplied by the donor. The flat portion can arise from a rapid decrease in the viscous time in the supercritical or radiative disk zones. The flat spectrum is associated with the variability of the X-ray jets that are formed in the supercritical disk region. 相似文献
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