Accretion in compact binaries

King, Andrew

doi:10.1017/cbo9780511536281.014

Cited by 15 publications

(9 citation statements)

References 67 publications

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“…[39,40]), attributed primarily to variations in the accretion rate. The accretion rate in turn varies on timescales of minutes to decades, with most notably, transient sources exhibiting outbursts during which the accretion rate increases by several orders of magnitude compared to the quiescent level [41]. As a result, GW searches for LMXB systems are necessarily limited to a coherence time equal to the maximum timescale over which the spin evolution can be well modelled.…”

Section: Scorpius X-1mentioning

confidence: 99%

Gravitational waves from Scorpius X-1: A comparison of search methods and prospects for detection with advanced detectors

et al. 2015

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The low-mass X-ray binary Scorpius X-1 (Sco X-1) is potentially the most luminous source of continuous gravitational-wave radiation for interferometers such as LIGO and Virgo. For low-mass X-ray binaries this radiation would be sustained by active accretion of matter from its binary companion. With the Advanced Detector Era fast approaching, work is underway to develop an array of robust tools for maximizing the science and detection potential of Sco X-1. We describe the plans and progress of a project designed to compare the numerous independent search algorithms currently available. We employ a mockdata challenge in which the search pipelines are tested for their relative proficiencies in parameter estimation, computational efficiency, robustness, and most importantly, search sensitivity. The mock-data challenge data contains an ensemble of 50 Scorpius X-1 (Sco X-1) type signals, simulated within a frequency band of 50-1500 Hz. Simulated detector noise was generated assuming the expected best strain sensitivity of Advanced LIGO [1] and Advanced VIRGO [2] (4 × 10 −24 Hz −1=2 ). A distribution of signal amplitudes was then chosen so as to allow a useful comparison of search methodologies. A factor of 2 in strain separates the quietest detected signal, at 6.8 × 10 −26 strain, from the torque-balance limit at a spin frequency of 300 Hz, although this limit could range from 1.2 × 10 −25 (25 Hz) to 2.2 × 10 −26 (750 Hz) depending on the unknown frequency of Sco X-1. With future improvements to the search algorithms and using advanced detector data, our expectations for probing below the theoretical torque-balance strain limit are optimistic.

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Section: Scorpius X-1mentioning

confidence: 99%

Gravitational waves from Scorpius X-1: A comparison of search methods and prospects for detection with advanced detectors

et al. 2015

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“…We refer to monographs by Frank, King & Raine [113] and Kato, Fukue & Mineshige [170] for exposition of accretion theory, to Krolik [188] and Peterson [273] for discussion of accretion flows with the emphasis on active galactic nuclei, and to various review papers [7,73,174,209,266] summarizing recent advances as well as the problems encountered by traditional scenarios.…”

Section: Introductionmentioning

confidence: 99%

Gravitating discs around black holes

Karas

Huré

Semerák

2004

Class. Quantum Grav.

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Abstract. Fluid discs and tori around black holes are discussed within different approaches and with the emphasis on the role of disc gravity. First reviewed are the prospects of investigating the gravitational field of a black hole-disc system by analytical solutions of stationary, axially symmetric Einstein's equations. Then, more detailed considerations are focused to middle and outer parts of extended disc-like configurations where relativistic effects are small and the Newtonian description is adequate.Within general relativity, only a static case has been analysed in detail. Results are often very inspiring, however, simplifying assumptions must be imposed: ad hoc profiles of the disc density are commonly assumed and the effects of frame-dragging and completely lacking. Astrophysical discs (e.g. accretion discs in active galactic nuclei) typically extend far beyond the relativistic domain and are fairly diluted. However, self-gravity is still essential for their structure and evolution, as well as for their radiation emission and the impact on the environment around. For example, a nuclear star cluster in a galactic centre may bear various imprints of mutual star-disc interactions, which can be recognised in observational properties, such as the relation between the central mass and stellar velocity dispersion.

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“…How ever, it is possible that a significant fraction of the LMXB population are transient, spending most of their lifecycle in quiescence (King [25]; van Paradijs [26] [27,28]. We take the initial mass function of Kroupa, Tout, & Gilmore [29] for the mass of the primary star (of mass M 1 ).…”

Section: Resultsmentioning

confidence: 99%

The low-mass X-ray binary-millisecond radio pulsar birthrate problem revisited

Dai

2010

Sci. China Phys. Mech. Astron.

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We investigate the birthrate problem for low-mass X-ray binaries (LMXBs) and millisecond radio pulsars (MRPs) in this paper. We consider intermediate-mass and low-mass X-ray binaries (I/LMXBs) to be the progenitors of MRPs, and calculate their evolutionary response to the cosmic star formation rate (SFR) both semi-analytically and numerically. With a typical value (1 Gyr) of the LMXB lifetime, one may expect comparable birthrates of LMXBs and MRPs, but the calculated number of LMXBs is an order of magnitude higher than that observed in the Galaxy. Instead, we suggest that the birthrate problem could be solved if most MRPs have evolved from faint to rather than bright LMXBs. The former may have a population of 10 4 in the Galaxy.close binaries, general pulsars, star formation, X-ray stars

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Accretion in compact binaries

Cited by 15 publications

References 67 publications

Gravitational waves from Scorpius X-1: A comparison of search methods and prospects for detection with advanced detectors

Gravitational waves from Scorpius X-1: A comparison of search methods and prospects for detection with advanced detectors

Gravitating discs around black holes

The low-mass X-ray binary-millisecond radio pulsar birthrate problem revisited

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