Fig. 7: Eccentricity and GW strain of dynamical NS–BH mergers.
From: Dissecting the properties of neutron star–black hole mergers originating in dense star clusters
a Mergers eccentricity distribution. The plot shows the eccentricity distribution for all mergers for the configuration with a single neutron star and a black hole–star binary (BHSTNS) assuming a metallicity value typical of old star clusters (Z = 0.0002) and a velocity dispersion σ = 100 km s−1. Different colors correspond to different frequency bands, namely 10−3 (millihertz, mHz), 10−2 (centihertz, cHz), 10−1 (decihertz, dHz), 100 (hertz, Hz), and 101 (decahertz, DHz). The eccentricity is measured as the merger crosses such bands. b Mergers GWs strain. Characteristic strain as a function of frequency for all mergers with a total merger time smaller than 105 years. Color-coding marks the eccentricity (e) variation. All colored tracks are assumed to be located at a luminosity distance of DL = 230 Mpc (redshift = 0.05). The characteristic strain for one single example is also shown assuming the source is located in the Virgo Cluster (red straight line) or in the Andromeda Galaxy (orange straight line).
