High-frequency quasi-periodic oscillations in black hole binaries

By T. Belloni, Andrea P. Sanna, M. Méndez. 2012

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We present the results of the analysis of a large data base of X-ray observations of 22 galactic black hole transients with the Rossi X-Ray Timing Explorer throughout its operative life for a total exposure time of similar to 12 ms. We excluded persistent systems and the peculiar source GRS 1915+105, as well as the most recently discovered sources. The semi-automatic homogeneous analysis was aimed at the detection of high-frequency (1001000?Hz) quasi-periodic oscillations (QPO), of which several cases were previously reported in the literature. After taking into account the number of independent trials, we obtained 11 detections from two sources only: XTE J1550-564 and GRO J1655-40. For the former, the detected frequencies are clustered around 180? and 280?Hz, as previously found. For the latter, the previously reported dichotomy 300450?Hz is found to be less sharp. We discuss our results in comparison with kHz QPO in neutron-star X-ray binaries and the prospects for future timing X-ray missions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7ee16625b0a38f3799de763920183352fcd44c05

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Citations in the corpus

Influence of Cosmic Repulsion and Magnetic Fields on Accretion Disks Rotating around Kerr Black Holes (2020, background): “The twin HF QPOs are two peaks of the X-ray power density observed in the case of microquasars in the frequency range ν ∼ 100–400 Hz; we can thus assume their creation in the innermost parts of the Keplerian accretion disks as the observed frequencies are close to the frequency of the orbital Kepler”
Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares (2018, methodology): “3Note that stellar QPPs are not to be confused with Quasi-Periodic Oscillations (QPOs) which is a term used in the astrophysical literature in relation to X-ray binaries (e.g. Lewin et al. 1988; Stella and Vietri 1998) and black hole binaries (e.g. Belloni et al. 2012).”
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets (2013, methodology): “Two other methods for measuring the spins of stellar black holes appear promising, namely, via X-ray polarimetry (Dovˇciak et al. 2008; Li et al. 2009; Schnittman & Krolik 2009) and high-frequency quasiperiodic oscillations (T¨or¨ok et al. 2005; Remillard & McClintock 2006; Belloni et al. 2012).”
Precise mass and spin measurements for a stellar-mass black hole through X-ray timing: the case of GRO J1655-40 (2013, methodology): “Lists of the HFQPOs detected in GRO J1655−40 are reported in Remillard et al. (1999), Strohmayer (2001) and Belloni et al. (2012).”
The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes (2014, background): “Note that there is some evidence that the frequencies can change by at least several percent [307, 308], which might be caused by the inner disk becoming marginally optically thin in some circumstances [309]), even in distinct outbursts separated by several years (XTE J1550−564 is one such case; see”