Gravitational-wave detection rates for compact binaries formed in isolation: LIGO/Virgo O3 and beyond

Abstract

Using simulations performed with the population synthesis code MOBSE, we compute the merger rate densities and detection rates of compact binary mergers formed in isolation for second-and third-generation gravitational-wave detectors. We estimate how rates are affected by uncertainties on key stellar-physics parameters, namely common envelope evolution and natal kicks. We estimate how future upgrades will increase the size of the available catalog of merger events, and we discuss features of the merger rate density that will become accessible with third-generation detectors.

Excitation of f -modes during mergers of spinning binary neutron star

“…(32) holds generically [as we discussed in Eqs. (22) and (23)]. To generalize the result to a realistic EOS, one only needs to replace the values of λ 0 and λ 2 accordingly-our equation of motion is an effective theory for the evolution of binary systems (without relativistic corrections).…”

“…Furthermore, 3G detectors, like the Einstein Telescope (ET) [19,20] and the Cosmic Explorer (CE) [21], are being planned for operation in the 2030s. These 3G detectors may increase neutron star black-hole and BNS detection rates by 3-4 orders of magnitude [22]. As a result, accurately modeling NSs in binary systems is necessary and timely.…”

Distinguishing double neutron star from neutron star-black hole binary populations with gravitational wave observations

“…There are large uncertainties in current estimates of BNS and stellar BHNS merger rates (see, e.g., [80]) and in key parameters of some of the more "exotic" formation scenarios, such as the fraction of dark matter in PBHs f PBH (see, e.g., [81][82][83][84][85][86]), but it is reasonable to expect that BNS merger rates should be larger than BHNS merger rates in the mass range of interest here. LIGO-Virgo observations have measured a 90% credible rate (to the nearest significant figure) of 100-4000 yr −1 Gpc −3 for BNS mergers, while the upper limit (in the absence of any candidates) on BHNS binaries is 600 yr −1 Gpc −3 [87,88].…”

Multiparameter Tests of General Relativity Using Multiband Gravitational-Wave Observations

“…Here, we consider 5 × 10 5 BBHs corresponding to one year of CE observation [33], distributed uniformly in comoving volume up to redshift z = 10. The primary black hole masses are assumed to follow a power-law distribution with the powerlaw index α = 1.6 (i.e., p(m 1 ) ∝ m −α 1 ) in the mass range [5, 100]M while secondary masses are uniform in the same mass range [34].…”