The jets and disc of SS 433 at super-Eddington luminositiesстатья

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

Работа с статьей

[1] Okuda T., Lipunova G. V., Molteni D. The jets and disc of ss 433 at super-eddington luminosities // Monthly Notices of the Royal Astronomical Society. — 2009. — Vol. 398, no. 4. — P. 1668–1677. We examine the jets and the disc of SS 433 at super-Eddington luminosities with (M) over dot similar to 600(M) over dot(c) by time-dependent two-dimensional radiation hydrodynamical calculations, assuming an alpha-model for the viscosity. One-dimensional supercritical accretion disc models with mass loss or advection are used as the initial configurations of the disc. As a result, from the initial advective disc models with alpha = 0.001 and 0.1, we obtain total luminosities similar to 2.5 x 1040 and 2.0 x 1040 erg s(-1). The total mass-outflow rates are similar to 4 x 10(-5) and 10(-4)M(circle dot) yr(-1), and the rates of the relativistic axial outflows in a small half opening angle of similar to 1 degrees are about 10(-6)M(circle dot) yr(-1): the values are generally consistent with the corresponding observed rates of the wind and the jets, respectively. From the initial models with mass loss but without advection, we obtain total mass-outflow and axial outflow rates smaller than or comparable to the observed rates of the wind and the jets, respectively, depending on alpha. In the advective disc model with alpha = 0.1, the initially radiation-pressure-dominant, optically thick disc evolves to a gas-pressure-dominated, optically thin state in the inner region of the disc, and the inner disc is unstable. Consequently, we find remarkable modulations of the disc luminosity and the accretion rate through the inner edge. These modulations manifest themselves as recurrent hot blobs with high temperatures and low densities at the disc plane, which develop outwards and upwards and produce quasi-periodic oscillations (QPOs) of the total luminosity with an amplitude of a factor of similar to 2 and quasi-periods of similar to 10-25 s. This may explain the massive jet ejection and the QPO phenomena observed in SS 433. [ DOI ]

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