Gravitational-Wave Astronomy

Press, William H.; Thorne, Kip S.

doi:10.1146/annurev.aa.10.090172.002003

Cited by 164 publications

(91 citation statements)

References 39 publications

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“…where d is the distance, h + and h × are dimensionless functions for the amplitude of the wave in two orthogonal polarizations, and dots denote time derivatives (Isaacson 1968;Press & Thorne 1972;Evans et al 1987). Assuming a binary system in a circular orbit of period P orb at a distance d, h + and h × are given by…”

Section: The Gw Signal From a Binary Starmentioning

confidence: 99%

The gravitational wave signal from diverse populations of double white dwarf binaries in the Galaxy

Jeffery

2010

A&A

130

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Context. The gravitational wave (GW) background in the range 0.01−30 mHz has been assumed to be dominated by unresolved radiation from double white dwarf binaries (DWDs). Recent investigations indicate that, at short periods, a number of DWDs should be resolvable sources of GW. Aims. We characterize the GW signal which would be detected by LISA from DWDs in the Galaxy. Methods. We have constructed a Galactic model in which we consider distinct contributions from the bulge, thin disc, thick disc, and halo, and subsequently executed a population synthesis approach to determine the birth rates, numbers, and period distributions of DWDs within each component. Results. In the Galaxy as a whole, our model predicts the current birth rate of DWDs to be 3.21 × 10 −2 yr −1 , the local density to be 2.2 × 10 −4 pc −3 and the total number to be 2.76 × 10 8 . Assuming SNIa are formed from the merger of two CO white dwarfs, the SNIa rate should be 0.0013 yr −1 . The frequency spectra of DWD strain amplitude and number distribution are presented as a function of galactic component, DWD type, formation channel, and metallicity. Conclusions. We confirm that CO+He and He+He white dwarf (WD) pairs should dominate the GW signal at very high frequencies (log f Hz −1 > −2.3), while CO+CO and ONeMg WD pairs have a dominant contribution at log f Hz −1 ≤ −2.3. Formation channels involving two common-envelope (CE) phases or a stable Roche lobe overflow phase followed by a CE phase dominate the production of DWDs detectable by LISA at log f Hz −1 > −4.5. DWDs with the shortest orbital periods will come from the CE+CE channel. The Exposed Core plus CE channel is a minor channel. A number of resolved DWDs would be detected, making up 0.012% of the total number of DWDs in the Galaxy. The majority of these would be CO+He and He+He pairs formed through the CE+CE channel.

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Section: The Gw Signal From a Binary Starmentioning

confidence: 99%

The gravitational wave signal from diverse populations of double white dwarf binaries in the Galaxy

Jeffery

2010

A&A

130

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“…It is important to appreciate that these formulas apply to strong-field sources as well as to weak field sources [43,44] as long as the relevant components of the effective stress energy tensor can be identified. Since in the present paper, we are only concerned with orbital motion of equal mass binaries, the multipole expansions reduce to only a few nonzero terms.…”

Section: E Gravitational Radiationmentioning

confidence: 99%

Relativistic numerical model for close neutron-star binaries

1996

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We describe a numerical method for calculating the (3+1) dimensional general relativistic hydrodynamics of a coalescing neutron-star binary system. The relativistic field equations are solved at each time slice with a spatial 3-metric chosen to be conformally flat. Against this solution to the general relativistic field equations the hydrodynamic variables and gravitational radiation are allowed to respond. The gravitational radiation signal is derived via a multipole expansion of the metric perturbation to the hexadecapole (l = 4) order including both mass and current moments and a correction for the slow motion approximation. Using this expansion, the effect of gravitational radiation on the system evolution can also be recovered by introducing an acceleration term in the matter evolution. In the present work we illustrate the method by applying this model to evaluate various orbits of two neutron stars with a gravitational mass of 1.45 M⊙ near the time of the final merger. We discuss the evidence that, for a realistic neutron star equation of state, general relativistic effects may cause the stars to individually collapse into black holes prior to merging. Also, the strong fields cause the last stable orbit to occur at a larger separation distance and lower frequency than previously estimated.PACS Numbers: 04.20.Jb, 04.30.+x, 47.75+f,, 95.30.Lz, 95.30.Sf 97.60.Jd,

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“…This discovery, along with emerging astrophysical understanding [22], led to the recognition that direct observations of the amplitude and phase of gravitational waves would enable studies of additional relativistic systems and provide new tests of general relativity, especially in the dynamic strong-field regime.…”

Section: Introductionmentioning

confidence: 99%

Observation of Gravitational Waves from a Binary Black Hole Merger

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Centennial of General Relativity

811

1,038

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On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 × 10 −21 . It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410 These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

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Gravitational-Wave Astronomy

Cited by 164 publications

References 39 publications

The gravitational wave signal from diverse populations of double white dwarf binaries in the Galaxy

The gravitational wave signal from diverse populations of double white dwarf binaries in the Galaxy

Relativistic numerical model for close neutron-star binaries

Observation of Gravitational Waves from a Binary Black Hole Merger

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