List of Footnotes

1 The hydrogen burning time for single stars with M0 ≲ 0.9M ⊙ exceeds the age of the Universe.
2 Unless the companion is directly observable and its mass can be estimated by other means.
3 Burst And Transient Source Experiment [21].
4 A signal with such an increasing frequency is reminiscent of the chirp of a bird. This explains the origin of the term “chirp mass” for the parameter ℳ which fully determines the GW frequency and amplitude behaviour.
5 For the first supernova explosion without kick this is always satisfied.
6 Instead of Monte Carlo simulations one may use a sufficiently dense grid in the 3D space of binary parameters and integrate over this grid (see, e.g., [423Jump To The Next Citation Point] and references therein).
7 Note that similar low values of λ for 20 to 50M ⊙ stars were obtained also by [322]. If confirmed, these results may have major impact on the estimates of merger rates for relativistic binaries.
8 If a network of three detectors, such as two LIGOs and VIRGO, runs simultaneously, the S∕N ratio in an individual detector should be √- > 7∕ 3 ≈ 4)
9 Flickering is a fast intrinsic brightness scintillation occurring on time scales from seconds to minutes with amplitudes of 0.01 – 1 mag and suggesting an ongoing mass transfer.
10 Remarkably, a clear-cut confirmation of the binary nature of AM CVn and the determination of its true period awaited for almost 25 years [282].
11 The recent discovery of SN Ia SN 2003fg with a mass estimate ∼ 2M ⊙ [154Jump To The Next Citation Point, 174Jump To The Next Citation Point] may support this scenario.
12 All these caveats date back as far as to MacDonalds’ 1984 paper [244] but are still not resolved.
13 The recently discovered hydrogen-rich SN Ia 2001ic and similarly 1997cy [132] may belong to the so-called SN 1.5 type or occur in a symbiotic system [58].
14 The reported discovery of Tycho Brahe’s 1572 SN Ia companion [361] is not confirmed as yet.
15 These numbers, like also for models discussed below, represent one random realization of the model and are subject to Poisson noise.
16 This is true for short-period systems, but becomes an oversimplification at longer periods and for Porb ≳ 40 min heating of the WD by accretion has to be taken into account [35].