Open AccessShock oscillation model for quasi‐periodic oscillations in stellar mass and supermassive black holes
Author(s) -
Okuda T.,
Teresi V.,
Molteni D.
Publication year - 2007
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 - 10.1111/j.1365-2966.2007.11736.x
Subject(s) - physics , astrophysics , accretion (finance) , supermassive black hole , shock wave , oscillation (cell signaling) , stellar mass , luminosity , outflow , black hole (networking) , active galactic nucleus , astronomy , stars , star formation , galaxy , mechanics , computer network , routing protocol , routing (electronic design automation) , biology , meteorology , computer science , genetics , link state routing protocol
We numerically examine centrifugally supported shock waves in 2D rotating accretion flows around a stellar mass (10 M ⊙ ) and a supermassive (10 6 M ⊙ ) black holes over a wide range of input accretion rates of . The resultant 2D shocks are unstable with time and the luminosities show quasi‐periodic oscillations (QPOs) with modulations of a factor of 2–3 and with periods of a tenth of a second to several hours, depending on the black hole masses. The shock oscillation model may explain the intermediate frequency QPOs with 1–10 Hz observed in the stellar mass black hole candidates and also suggest the existence of QPOs with the period of hours in active galactic nuclei. When the accretion rate is low, the luminosity increases in proportion to the accretion rate. However, when greatly exceeds the Eddington critical rate , the luminosity is insensitive to the accretion rate and is kept constantly around ∼3 L E . On the other hand, the mass‐outflow rate increases in proportion to and it amounts to about a few per cent of the input mass‐flow rate.