Table 1.
Merger rate results for compact binaries containing a white dwarf and a neutron star–black hole.
| Verbunt et al. (2017) | Hobbs et al. (2005) | Bray & Eldridge (2016) | |||||||
|---|---|---|---|---|---|---|---|---|---|
| Binary | fmerge | fbin | log10(N/M⊙) | fmerge | fbin | log10(N/M⊙) | fmerge | fbin | log10(N/M⊙) |
| Z = 0.5 Z⊙ | |||||||||
| WD1-NS2 | 0.03 | 0.22 | −6.52 | 0.10 | 0.28 | −6.56 | 0.01 | 0.14 | −6.69 |
| NS1-WD2 | 10−2.5 | 0.78 | −5.98 | 0.01 | 0.72 | −6.14 | 10−2.6 | 0.86 | −5.92 |
| WD1-BH2 | – | – | – | – | – | – | – | – | – |
| BH1-WD2 | 10−3.3 | 1.00 | −7.18 | 10−2.9 | 1.00 | −7.11 | 10−3.3 | 1.00 | −6.97 |
| Z = 0.2 Z⊙ | |||||||||
| WD1-NS2 | 0.03 | 0.12 | −6.38 | 0.14 | 0.23 | −6.17 | 0.01 | 0.05 | −6.63 |
| NS1-WD2 | 0.01 | 0.88 | −5.52 | 0.02 | 0.77 | −5.64 | 0.01 | 0.95 | −5.37 |
| WD1-BH2 | – | – | – | – | – | – | – | – | – |
| BH1-WD2 | 10−3.4 | 1.00 | −7.13 | 10−3.4 | 1.00 | −7.35 | 10−3.2 | 1.00 | −6.71 |
Notes. Results are shown for the three natal kick prescriptions (Verbunt, Hobbs, and Bray, left to right), and both metallicities considered in this work (0.5 Z⊙ above the horizontal line, 0.2 Z⊙ below it). fmerge is the fraction of binaries from each formation pathway that merge within a Hubble time. fbin is the fraction of mergers within a Hubble time, for each class of binary (e.g. WDNS), arising from each pathway within that class (e.g. NS1-WD2). We also list the number of mergers from each pathway in a Hubble time, per solar mass of stars formed. Although they dominate mergers within a Hubble time, at ages ≲10 Gyr, the direct (NS1 and BH1) channels are negligible and the reverse channel dominates. The WD1 pathways are therefore over-represented in the GRB host stellar populations studied in this work, which are < 10 Gyr old (see Figure 3).
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