Free Access

Table 1

Summary of the key parameters adopted in our standard simulations and the variations that we consider.

Symbol Standard modelsa Model variations

Physical assumptions
- Mass transfer efficiency β 0, 0.2, 1
- Angular momentum loss γ γorb,acc 0, γdisk
- Mass loss during merger of two MS stars μloss 0.1 0, 0.25
- Mixing during merger of two MS stars μmix 0.1 0, 1
- Natal kick compact remnant (km s-1) σ 265 σ0,
- Common envelope efficiency αCE 1 0.1, 0.2, 0.5, 2, 5, 10
- Envelope binding energy λCE λDewi + 00 0.5
- Critical mass ratio for contact for MS donor qcrit,MS 0.65 0.25, 0.8
- Critical mass ratio for unstable mass transfer for HG donor qcrit,HG 0.4 0, 0.25, 0.8, 1
- Stellar-wind mass-loss efficiency parameter η 1 0.33, 3
- Maximum single-star equivalent birth mass for ccSN (M) M max,cc 100 20, 35
- Minimum metal core for ccSN (M) M min,metal 1.37 1.3, 1.4
Initial conditions
- Slope initial mass function α −2.3 –1.6, –2.7, –3.0
- Slope initial mass ratio distribution κ 0 –1, 1
- Slope of initial period distr. π π Opik24, Sana + 12 –1, 1
- Metallicity Z 0.014 0.0002, 0.004, 0.008, 0.02, 0.03
- Binary fractiona f bin 0.7, 0.0a 0.3, 1,
- Normalization parameter (M) Mlow 2 1, 3

Notes. See Sect. 2 for a description of the symbols and further assumptions.

(a)

The difference between our two standard models is that in one we simulate only single stars and in the other we assume a binary fraction of 0.7.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.