Open AccessQuasi‐periodic oscillation frequencies and mass‐outflow rates in black hole powered Galactic microquasars
Author(s) -
Das Tapas K.,
Rao A. R.,
Vadawale Santosh V.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06688.x
Subject(s) - physics , astrophysics , accretion (finance) , outflow , black hole (networking) , hydrostatic equilibrium , shock wave , active galactic nucleus , schwarzschild metric , oscillation (cell signaling) , astronomy , general relativity , classical mechanics , galaxy , mechanics , computer network , routing protocol , routing (electronic design automation) , biology , genetics , link state routing protocol , meteorology , computer science
For all available pseudo‐Schwarzschild potentials, we provide a non ‐self‐similar model of coupled accretion–outflow systems in connection with the quasi‐periodic oscillation (QPO) of black hole powered Galactic microquasars and the emergence of baryonic jets from these objects. We use the vertically integrated 1.5‐dimensional model to describe the disc structure where the equations of motion are written for the equatorial plane of the central accretor, assuming the flow to be in hydrostatic equilibrium in the transverse direction. First we formulate and solve the equations governing axisymmetrically rotating, advective, multitransonic black hole accretion, which may contain Rankine–Hugoniot shock waves, and then we calculate the associated QPO frequencies ν QPO in terms of relevant accretion parameters. We then argue that the post‐shock region for such flows may serve as an efficient source of outflow generation; and we calculate, for the same set of accretion parameters used to calculate the QPO frequencies, what fraction of the accreting material, denoted by , is being blown as shock‐generated outflow. In this way we theoretically study the relation between ν QPO and for Galactic microquasars and compare our theoretically obtained result with observational data.