A Practical Theorem on Gravitational Wave Backgrounds

By E. Phinney. 2001

251 citations recorded by the source corpus.

There is an extremely simple relationship between the spectrum of the gravitational wave background produced by a cosmological distribution of discrete gravitational wave sources, the total time-integrated energy spectrum of an individual source, and the present-day comoving number density of remnants. Stated in this way, the background is entirely independent of the cosmology, and only weakly dependent on the evolutionary history of the sources. This relationship allows one easily to compute the amplitude and spectrum of cosmic gravitational wave backgrounds from a broad range of astrophysical sources, and to evaluate the uncertainties therein.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/711f15f7a7c08be3746ef9107dfa357aabaf9882

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Citations in the corpus

Gravitational waves from primordial black hole mergers (2017, background): “ary formation but used a xed rate. 4.1 Constraints from the non-observation of the GW background PBH mergers occurring with a dierential rate dR(z) yield a stochastic GW background with the spectrum [58,63] GW() = ˆ c Z dzdR(z) 1 (1 + z)H(z) dE GW( r) d ; (4.1) { 10 { where ˆ c = 3H2 0 =8ˇGdenotes ”
Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays (2008, background): “The possible level of the GW background, and the consequences for observations have been explored by several authors (see e.g. Rajagopal & Romani 1995; Phinney 2001, Jaffe & Backer 2003; Jenet et al. 2005; Jenet et al. 2006; Sesana et al. 2008).”
Science with the space-based interferometer LISA. IV: probing inflation with gravitational waves (2016, background): “ed a xed merger rate of 50 events per year and Gpc3. The gravitational wave background from inspiraling black holes can be obtained straightforwardly from the GWs emission of binary systems, see ref. [164], GW(f) = 2ˇ2 3H2 0 f2 h2 c(f) 1 ˆ c dˆ GW dlnf ; (6.24) where dˆ GW dlnf = Z 1 0 dz 1 + z dn ”
TianQin: a space-borne gravitational wave detector (2015, background): “ly does such a contribution have a low probability, but given the matched-lter approach that will be used to study the reference source, any such contribution would be small and easily accounted for [50]. The relevant analysis is ongoing and will be reported elsewhere. The preliminary error budget o”
The astrophysics of nanohertz gravitational waves (2018, methodology): “This is calculated by integrating the squared GW strain signal over the entire emitting population (Phinney 2001).”