Physics, Astrophysics and Cosmology with Gravitational Waves

By B. Sathyaprakash, Bernard F. Schutz. Living Reviews in Relativity, 2009

793 citations recorded by the source corpus.

Gravitational wave detectors are already operating at interesting sensitivity levels, and they have an upgrade path that should result in secure detections by 2014. We review the physics of gravitational waves, how they interact with detectors (bars and interferometers), and how these detectors operate. We study the most likely sources of gravitational waves and review the data analysis methods that are used to extract their signals from detector noise. Then we consider the consequences of gravitational wave detections and observations for physics, astrophysics, and cosmology.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d546af4909d6ea8f55298371dabc0e06582a993c

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Citations in the corpus

• Origin of the Chemical Elements (2010, background): “…be able to study another type of radiation in addition to the electromagnetic one: gravitational waves emitted, e.g., by neutron star mergers, black hole formation, and other interactions between highly massive or Origin of the Chemical Elements relativistic objects (Sathyaprakash and Schutz 2009).”
• Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, background): “Mergers are also loud gravitational-wave (GW) sources and one of the targets for the nascent field of GW astronomy (Sathyaprakash & Schutz 2009), recently inaugurated with the detection of GWs from a pair of merging BHs (Abbott et al. 2016).”
• Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave (2014, background): “…waves are easier to detect, since the detectable distance is proportional to 5/6 power of the chirp mass (Mchirp) of a binary defined by Mchirp = (M1M2)3/5/(M1 + M2)1/5 (Peters & Mathews 1963; Peters 1964, see also Sathyaprakash & Schutz 2009), where M1 and M2 are the mass of each compact object.”
• Squeezed states of light and their applications in laser interferometers (2016, background): “A variety of known astrophysical and cosmological sources are predicted to emit gravitational radiation that should reach the Earth with a measurable strength [Sathyaprakash and Schutz (2009)]. The first gravitational wave event detected was produced by two black holes of 36 and 29 solar masses. Dur”
• Gravitational-wave sensitivity curves (2014, methodology): “BO) and Deci-hertz Interferometer GW Observatory (DECIGO) are designed to probe decihertz GWs. 4.3.1. LISA and eLISA The instrumental noise curves for LISA are approximated by the analytic t given by Sathyaprakash and Schutz (2009), which we use for the plots in Appendix A. When observing individual”
• Gravitational Radiation Detection with Laser Interferometry (2013, background): “Previous overviews (Cutler and Thorne, 2002; Hawking and Israel, 1989) have covered the list of known sources as well as describing the astrophysical and cosmological science that can be extracted from them(Sathyaprakash and Schutz, 2009).”