List of Footnotes
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3 | The existence of such high-mass very short-living objects is deemed possible due to runaway stellar collisions in dense young compact stellar clusters [605]; for the prospects of observing them see, e.g., [564]. | |
4 | AGB – Asymptotic Giant Branch on the Hertzsprung–Russell diagram | |
5 | TP-AGB – thermally pulsing AGB, the late stage of the AGB evolution, characterized by the development of strong pulsations leading ultimately to the ejection of the entire envelope of the red giant star. | |
6 | Yet another possibility for the formation of neutron stars exists: if a sufficiently cold white dwarf close to critical mass accretes matter, the time scale of its gravitational collapse allows neutronization before the onset of pycnonuclear reactions [85]. | |
7 | See these papers for detailed references and discussion of earlier studies. | |
8 | Results obtained by the same group for lower metallicities may be found in Poelarend’s PhD thesis at
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9 | Pair-creation instability in the oxygen cores of slowly rotating ![]() ![]() ![]() ![]() |
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10 | To compare the detector’s sensitivity, characterized by the noise power spectral density ![]() ![]() ![]() ![]() ![]() |
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11 | Unless the companion is directly observable and its mass can be estimated by other means. | |
12 | We neglect here the highly unlikely case of a direct collision between a newly born BH and its companion due to the possible BH natal kick. | |
13 | 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 ![]() |
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14 | Actually, no CVs were known in the “gap” when this fact was first realized [647]. | |
15 | Actually, the Roche potential should also incorporate the effects of radiation pressure from the binary components. Then in some cases the resulting potentials do not exhibit the contact surfaces of the classical Roche potential [684, 144]. | |
16 | Hydrogen burning time for solar-composition single stars with ![]() |
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17 | In principle, it is possible to form a close binary system with a compact star (NS or BH) from a hierarchical triple system without an initial CE phase due to dynamical interactions (Kozai–Lidov mechanism), see [693]. | |
18 | Indeed, to put a gas element of unit mass with specific volume ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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19 | Attempts to apply the ![]() ![]() ![]() |
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20 | Tutukov and Yungelson’s paper [782] was published in 1973 prior to the discovery of the first pulsar binary PSR 1913+16 in 1974 [757, 292*] and, though the evolutionary path was traced to a NS (or BH) binary, since no such objects were known at that time, it was suggested that all pairs of NSs are disrupted at the second NS formation. | |
21 | For the first supernova explosion without kick this is always satisfied. | |
22 | 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., [791*] and references therein). | |
23 | Note that similar low values of ![]() ![]() ![]() |
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24 | If a network of three detectors, such as two LIGOs and VIRGO, runs simultaneously, the ![]() ![]() |
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25 | 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. | |
26 | Remarkably, a clear-cut confirmation of the binary nature of AM CVn and the determination of its true period awaited for almost 25 years [513]. | |
27 | It is expected that recently launched astrometric space mission GAIA will detect about 200 eclipsing double degenerates [511]. | |
28 | The advent of new, fast and stable stellar evolutionary codes like MESA [574, 575], ![]() |
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29 | Note that the existence of these winds has never been rigorously proven by radiative transfer theory. | |
30 | The latter is characterized by the parameter ![]() ![]() ![]() |
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31 | ![]() |
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32 | The “optimistic” model of the population of IDD was taken [512*], which assumes effective tidal interaction and inefficient destruction of hypothetical progenitors of AM CVn stars due to double-degenerate SN Ia. Thus, the numbers provided in the table are upper limits. | |
33 | These numbers, as for models discussed below, represent one random realization of the model and are subject to Poissonian noise. | |
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37 | This is true for long-period systems, but becomes an oversimplification at shorter periods and for ![]() |