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Table A.4.

Consequences from the common envelope channel.

a Pi(d)b Pf(min)c MsdB(M)d K(kms−1)e f0(Hz)f g t(Myr)h
3.2 10 25.92 0.3599 778.90 1.27887 × 10−3 1.48151 × 10−18 2.5938 × 100
20 59.04 0.3768 589.54 5.65211 × 10−4 1.17768 × 10−18 2.1931 × 101
30 96.48 0.3889 497.50 3.44314 × 10−4 1.02808 × 10−18 7.9857 × 101

4.0 12 20.16 0.4620 822.36 1.68480 × 10−3 2.04599 × 10−18 9.8716 × 10−1
20 36.00 0.4675 674.97 9.37043 × 10−4 1.70084 × 10−18 4.6680 × 100
35 67.68 0.4836 539.78 4.87594 × 10−4 1.41133 × 10−18 2.5831 × 101
50 109.44 0.4974 460.13 3.06448 × 10−4 1.24030 × 10−18 8.6871 × 101

5.0 30 33.12 0.6049 659.34 1.00674 × 10−3 2.20153 × 10−18 3.0505 × 100
40 43.20 0.6095 599.54 7.60428 × 10−4 2.01874 × 10−18 6.4026 × 100
50 56.16 0.6169 550.29 5.92342 × 10−4 1.87770 × 10−18 1.2329 × 101
60 70.56 0.6242 509.90 4.74609 × 10−4 1.76230 × 10−18 2.2031 × 101
70 86.40 0.6316 474.82 3.86063 × 10−4 1.66258 × 10−18 3.7808 × 101
80 103.68 0.6385 445.77 3.21636 × 10−4 1.57977 × 10−18 6.0924 × 101

Notes.

(a)

Initial mass of the MS star;

(b)

initial period of systems;

(c)

final period of systems;

(d)

mass of sdBs;

(e)

RV semi-amplitude of systems;

(f)

frequency of the GW;

(g)

root spectral density of the GW strain;

(h)

timescale of the merger.

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