Models (see the files at the bottom of the page) are from this paper

Sample results from one of our models are shown on the Figure below.

Detection weighted distribution of the effective spin parameter of BH-BH mergers for model M30.B with MESA efficient angular momentum transport and fallback decreased BH kicks (no BH kicks for massive BHs). We either do not allow for effcient tidal spin-up of WR stars that are the most common immediate progenitors of BHs in our models (natal BH spin is calculated directly from MESA stellar models), or we take it into account (natal BH spin is then calculated as described in Sec. 2.5 in (Belczynski et al. 2019) if the WR star progenitor was subject to an effcient tidal spin-up). For the "no WR tides" approach we find a rather narrow distribution of effective spins (-0.2 <~ Chi_eff <~ 0.2) that is peaked at positive values (average Chi_eff = 0.15). For effcient "WR tides" the distribution is broad (-0.5 <~ Chi_eff <~ 1.0) with a peak at Chi_eff ~ 0.15 (~72%) and a tail with Chi_eff >~ 0.25 (28%). For comparison we show the 90% credible limits (blue arrows) and the most likely values (blue stars) of the effective spin parameter for ten LIGO/Virgo BH-BH mergers.

Comparison of the local merger rate densities of BH-BH and BH-NS mergers from all our models (see Tables 3 and 4 in (Belczynski et al. 2019)) with the current limits: 9.7–101 Gpc^-3 yr^-1 for the BH-BH mergers (LIGO/Virgo O1/O2) and 1.3–35 Gpc^-3 yr^-1 for the BH-NS events (based on the LIGO/Virgo O3 candidate of the first BH-NS system, S190814bv (LVC 2019a,b); see Sec. 6.8 in (Belczynski et al. 2019) for details). Models consistent with the observational limits are: M13.A, M23.A, M33.A, M43.A, M23.B, M25.B, M26.B, M30.B, M40.B, M50.B, M60.B, M70.B. Note also that the BH-NS merger rates from our models span the range between 0.51 and 301 Gpc^-3 yr^-1, which is consistent with the upper limit determined by their non-detection in O1/O2 LIGO/Virgo runs (< 610 Gpc^-3 yr^-1, The LIGO Scientific Collaboration et al. (2018b)).

Comparison of the local merger rate densities of BH-BH and NS-NS mergers from all our models (see Tables 3 and 4 in (Belczynski et al. 2019)) with the current limits inferred from the O1/O2 LIGO/Virgo observational runs: 9.7–101 Gpc^-3 yr^-1 for the BH-BH mergers and 110–3840 Gpc^-3 yr^-1 for the NS-NS events (The LIGO Scientific Collaboration et al. 2018b). Models consistent with the observational limits are: M13.A, M23.A, M33.A, M43.A, M30.B, M40.B, M60.B, M70.B. Note that while some of the models are consistent with the observational constraints and others are not, it is not straightforward to draw conclusions about the physical ingredients of the models at this stage due to degeneracies in the impact of various assumptions on the theoretical merger rates (see Sect. 4.4.1 in (Belczynski et al. 2019)).

This website will be kept updated with new models and observations as they appear.

Please look here for the description of the results available below.

### m10

### m13

### m20

### m23

### m25

### m26

### m30

### m33

### m35

### m40

### m43

### m50

### m60

### m70