2006A&A...454..559Y


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.15CEST07:58:00

2006A&A...454..559Y - Astronomy and Astrophysics, volume 454, 559-569 (2006/8-1)

The origin and fate of short-period low-mass black-hole binaries.

YUNGELSON L.R., LASOTA J.-P., NELEMANS G., DUBUS G., VAN DEN HEUVEL E.P.J., DEWI J. and PORTEGIES ZWART S.

Abstract (from CDS):

We present results of a population synthesis study for semidetached short orbital period binaries which contain low-mass (≲1.5M) donors and massive (>4M) compact accretors, which in our model represent black holes. Evolution of these binaries is determined by nuclear evolution of the donors and/or orbital angular momentum loss due to magnetic braking by the stellar wind of the donors and gravitational wave radiation. According to our model the estimated total number of this type of black-hole binaries in the Galaxy is >10000. If the magnetic braking removing angular momentum in semidetached black-hole binaries is described by the Verbunt & Zwaan (1981A&A...100L...7V) formula, the model predicts that among them around 3000 systems with periods >2h would be transient. In addition one finds several hundreds of luminous and stable systems with periods between 3 and 8h. Several dozens of these bright systems should be observed above the RXTE ASM sensitivity limit. The absence of such systems implies that upon Roche-lobe overflow by the low-mass donor angular momentum losses are reduced by a factor more than 2 with respect to the Verbunt & Zwaan (1981A&A...100L...7V) prescription. In such a case short period black-hole soft X-ray transients (SXT) may have donors that overflow the Roche lobe in the core hydrogen-burning stage. We show that it is unlikely that the transient behaviour of black-hole short-period X-ray binaries is explained by the evolved nature of the stellar companion. On the other hand a substantial fraction of black-hole binaries with periods >3h could be faint with truncated, stable cold accretion discs as proposed by Menou et al. Most of the semidetached black-hole binaries are expected to have periods shorter than ∼2h. Properties of such, still to be observed, very small mass-ratio (q=M2/M1<0.02) binaries are different from those of their longer period cousins.

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Journal keyword(s): binaries: close - stars: evolution - X-rays: binaries

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SK 160 HXB 01 17 05.1447530244 -73 26 36.015353425 12.23 13.00 13.15   13.17 O9.7Ia+ 798 0
2 V* V518 Per HXB 04 21 42.7231318463 +32 54 26.936934166 13.00 13.50 13.2     M4.5V 620 1
3 1A 0620-00 HXB 06 22 44.5420315454 -00 20 44.289428950 10.60 11.40 11.2     K3V-K7V 1040 0
4 V* MM Vel HXB 10 13 36.4107940553 -45 04 32.555813596   14.84 14.71     G5V-M0V 183 0
5 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 721 0
6 V* GU Mus HXB 11 26 26.5947467816 -68 40 32.888148788           K3V-K7V 670 1
7 V* IL Lup HXB 15 47 08.2766679321 -47 40 10.284971214           ~ 412 1
8 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60           K4V 345 0
9 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1764 0
10 V* V2107 Oph HXB 17 08 14.520 -25 05 30.15   16.50 15.9     K3V-K7V 211 1
11 V* V406 Vul HXB 18 58 41.580 +22 39 29.40 15.00 15.65 15.31     G5V-K0V 316 0
12 Granat 1915+105 LXB 19 15 11.54938 +10 56 44.7585           ~ 2285 0
13 V* QZ Vul HXB 20 02 49.58 +25 14 11.3   19.64 18.2     K3V-K6V 398 0
14 V* V404 Cyg HXB 20 24 03.820 +33 52 01.90 14.50 14.20 12.7     K0IV 1090 0

    Equat.    Gal    SGal    Ecl

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2020.07.15-07:58:01

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