Shock oscillation model for quasi-periodic oscillations in stellar mass and supermassive black holes

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Abstract

We numerically examine centrifugally supported shock waves in 2D rotating accretion flows around a stellar mass (10 M) and a supermassive (106 M) black holes over a wide range of input accretion rates of 107 M˙ /M˙ E 10−4. 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 M˙ is low, the luminosity increases in proportion to the accretion rate. However, when M˙ greatly exceeds the Eddington critical rate M˙ E, the luminosity is insensitive to the accretion rate and is kept constantly around ∼3LE. On the other hand, the mass-outflow rate M˙ loss increases in proportion to M˙ and it amounts to about a few per cent of the input mass-flow rate
Lingua originaleEnglish
pagine (da-a)1431-1438
Numero di pagine8
RivistaMonthly Notices of the Royal Astronomical Society
Volume377
Stato di pubblicazionePublished - 2007

All Science Journal Classification (ASJC) codes

  • Space and Planetary Science

Cita questo

@article{f48d5d8ee2b949d2aa0c2a995a9f3b2f,
title = "Shock oscillation model for quasi-periodic oscillations in stellar mass and supermassive black holes",
abstract = "We numerically examine centrifugally supported shock waves in 2D rotating accretion flows around a stellar mass (10 M) and a supermassive (106 M) black holes over a wide range of input accretion rates of 107 M˙ /M˙ E 10−4. 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 M˙ is low, the luminosity increases in proportion to the accretion rate. However, when M˙ greatly exceeds the Eddington critical rate M˙ E, the luminosity is insensitive to the accretion rate and is kept constantly around ∼3LE. On the other hand, the mass-outflow rate M˙ loss increases in proportion to M˙ and it amounts to about a few per cent of the input mass-flow rate",
keywords = "accretion, accretion discs, black hole physics, hydrodynamics, radiation, mechanism: thermal, shock waves",
author = "Diego Molteni and Vincenzo Teresi and Toru Okuda",
year = "2007",
language = "English",
volume = "377",
pages = "1431--1438",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",

}

TY - JOUR

T1 - Shock oscillation model for quasi-periodic oscillations in stellar mass and supermassive black holes

AU - Molteni, Diego

AU - Teresi, Vincenzo

AU - Okuda, Toru

PY - 2007

Y1 - 2007

N2 - We numerically examine centrifugally supported shock waves in 2D rotating accretion flows around a stellar mass (10 M) and a supermassive (106 M) black holes over a wide range of input accretion rates of 107 M˙ /M˙ E 10−4. 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 M˙ is low, the luminosity increases in proportion to the accretion rate. However, when M˙ greatly exceeds the Eddington critical rate M˙ E, the luminosity is insensitive to the accretion rate and is kept constantly around ∼3LE. On the other hand, the mass-outflow rate M˙ loss increases in proportion to M˙ and it amounts to about a few per cent of the input mass-flow rate

AB - We numerically examine centrifugally supported shock waves in 2D rotating accretion flows around a stellar mass (10 M) and a supermassive (106 M) black holes over a wide range of input accretion rates of 107 M˙ /M˙ E 10−4. 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 M˙ is low, the luminosity increases in proportion to the accretion rate. However, when M˙ greatly exceeds the Eddington critical rate M˙ E, the luminosity is insensitive to the accretion rate and is kept constantly around ∼3LE. On the other hand, the mass-outflow rate M˙ loss increases in proportion to M˙ and it amounts to about a few per cent of the input mass-flow rate

KW - accretion, accretion discs, black hole physics, hydrodynamics, radiation, mechanism: thermal, shock waves

UR - http://hdl.handle.net/10447/7270

M3 - Article

VL - 377

SP - 1431

EP - 1438

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

ER -