Long-term operation of the Laser Interferometer Space Antenna and Galactic close white dwarf binaries

Seto, Naoki

doi:10.1046/j.1365-8711.2002.05432.x

Cited by 40 publications

(32 citation statements)

References 27 publications

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“…[285, 286]). The comparison with the work of other authors [141, 445, 374] shows that both the frequency of the confusion limit and the level of confusion noise are uncertain within a factor of ∼ 4. This uncertainty is clearly high enough to influence seriously the estimates of the possibilities for a detection of compact binaries.…”

Section: Gravitational Waves From Compact Binaries With White-dwarf Cmentioning

confidence: 59%

The Evolution of Compact Binary Star Systems

Постнов¹,

Yungelson

2006

Living Rev. Relativ.

121

114

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We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Binary NSs and BHs are thought to be the primary astrophysical sources of gravitational waves (GWs) within the frequency band of ground-based detectors, while compact binaries of WDs are important sources of GWs at lower frequencies to be covered by space interferometers (LISA). Major uncertainties in the current understanding of properties of NSs and BHs most relevant to the GW studies are discussed, including the treatment of the natal kicks which compact stellar remnants acquire during the core collapse of massive stars and the common envelope phase of binary evolution. We discuss the coalescence rates of binary NSs and BHs and prospects for their detections, the formation and evolution of binary WDs and their observational manifestations. Special attention is given to AM CVn-stars — compact binaries in which the Roche lobe is filled by another WD or a low-mass partially degenerate helium-star, as these stars are thought to be the best LISA verification binary GW sources.

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Section: Gravitational Waves From Compact Binaries With White-dwarf Cmentioning

confidence: 59%

The Evolution of Compact Binary Star Systems

Постнов¹,

Yungelson

2006

Living Rev. Relativ.

121

114

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“…Ϫ8/3 ( f /3 mHz) res (e.g., Hils et al 1990;Seto 2002 and references therein) above this frequency. Below there will be other individually ref res solved binaries, particularly those that are nearby, but here we focus on those above the resolution limit, as theoretical predictions of the resolved number are more reliable and parameter extractions are likely to be more useful for localizing the CWDB population.…”

Section: Introductionmentioning

confidence: 99%

The Optical Identification of Close White Dwarf Binaries in the Laser Interferometer Space Antenna Era

Cooray¹,

Farmer²,

Seto³

2004

ApJ

Self Cite

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The Laser Interferometer Space Antenna (LISA) is expected to detect close white dwarf binaries (CWDBs) through their gravitational radiation. Around 3000 binaries will be spectrally resolved at frequencies greater than 3 mHz, and their positions on the sky will be determined to an accuracy ranging from a few tens of arcminutes to a degree or more. Because of the small binary separation, the optical light curves of տ30% of these CWDBs are expected to show eclipses, giving a unique signature for identification in follow-up studies of the LISA error boxes. While the precise optical location improves binary parameter determination with LISA data, the optical light curve captures additional physics of the binary, including the individual sizes of the stars in terms of the orbital separation. To optically identify a substantial fraction of CWDBs and thus localize them very accurately, a rapid monitoring campaign is required, capable of imaging a square degree or more in a reasonable time, at intervals of 10-100 s, to magnitudes between 20 and 25. While the detectable fraction can be up to many tens of percent of the total resolved LISA CWDBs, the exact fraction is uncertain because of unknowns related to the WD spatial distribution and potentially interesting physics, such as induced tidal heating of the WDs due to their small orbital separation.

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“…Indeed, one of the probable reasons for this lack of theoretical models is the heavy computational demand involved in the simulation of an intrinsically three-dimensional phenomenon. However, in sharp contrast, the coalescence of two neutron stars has been extensively studied -see, for instance, Rosswog et al (2001) and Rosswog & Davies (2000, 2002, and references therein, for some of the most recent works on this subject.…”

Section: Introductionmentioning

confidence: 99%

“…Finally, the initial stages of the coalescence of a white dwarf binary system could be one of the most interesting sources for the detection of gravitational waves using Earth-based laser interferometers like LIGO (Abramovici et al 1992) or space-borne detectors like LISA (http://lisa.jpl.nasa.gov). In particular, Galactic close binary white dwarfs are expected to contribute significantly to the background noise (Evans et al 1987) during the spiraling phase and the merging process itself would produce a signal that could eventually be detected (Seto 2002).…”

Section: Introductionmentioning

confidence: 99%

Smoothed Particle Hydrodynamics simulations of merging white dwarfs

Guerrero

Garcı́a–Berro

Isern

2003

A&A

143

192

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Abstract. We present the results of three-dimensional Smoothed Particle Hydrodynamics (SPH) calculations of the process of coalescence of white dwarfs. We follow in detail the initial phase of the merging for several masses of the primary and the secondary of the binary system. Special attention has been paid to the issue of whether or not thermonuclear runaway occurs during the process of merging. We find that although relatively high temperatures are attained during the most violent phase of the merging process, the thermonuclear flash is rapidly quenched. The total mass lost by the system is also relatively small (of the order of 0.5% at most) except for the most massive primaries for which it is still small (∼2.2%). Consequently, a heavy accretion disk around the primary is formed. We also discuss the subsequent evolution of the resulting system and the possible astrophysical scenarios of interest.

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Long-term operation of the Laser Interferometer Space Antenna and Galactic close white dwarf binaries

Cited by 40 publications

References 27 publications

The Evolution of Compact Binary Star Systems

The Evolution of Compact Binary Star Systems

The Optical Identification of Close White Dwarf Binaries in the Laser Interferometer Space Antenna Era

Smoothed Particle Hydrodynamics simulations of merging white dwarfs

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