2008A&A...488..257Y


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.28CEST03:12:40

2008A&A...488..257Y - Astronomy and Astrophysics, volume 488, 257-265 (2008/9-2)

Evolutionary models of short-period soft X-ray transients: comparison with observations.

YUNGELSON L.R. and LASOTA J.-P.

Abstract (from CDS):

We consider evolutionary models for the population of short-period (Porb≲10h) low-mass black-hole binaries (LMBHBs) and compare them with observations of soft X-ray transients (SXTs). We show that assuming strongly reduced magnetic braking (as suggested by us before for low-mass semidetached binaries) the calculated masses and effective temperatures of secondaries are encouragingly close to the observed masses and effective temperatures (as inferred from their spectra) of donor stars in short-period LMBHBs. Theoretical mass-transfer rates in SXTs are consistent with the observed ones if one assumes that accretion discs in these systems are truncated (``leaky''). We find that the population of short-period SXTs is formed mainly by systems which had unevolved or slightly evolved main-sequence donors (M2≲1.2M) with a hydrogen abundance in the center Xc>0.35 at the Roche-lobe overflow (RLOF). Longer period (Porb≃(0.5-1)day) SXTs might descend from systems with initial donor masses of about 1M and Xc≲0.35. Thus, one can explain the origin of short period LMBHB without invoking donors with cores almost totally depleted of hydrogen. Our models suggest that, unless the currently accepted empirical estimates of mass-loss rates by winds for massive O-stars and Wolf-Rayet stars are significantly over-evaluated, a very high efficiency of common-envelope ejection is necessary to form short-period LMBHBs.

Abstract Copyright:

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

Status at CDS:  

Simbad objects: 12

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Number of rows : 12

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 NAME IC 10 X-1 HXB 00 20 29.09 +59 16 51.9           ~ 147 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 1037 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 718 0
6 V* GU Mus HXB 11 26 26.5947467816 -68 40 32.888148788           K3V-K7V 669 1
7 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60           K4V 345 0
8 V* V2107 Oph HXB 17 08 14.520 -25 05 30.15   16.50 15.9     K3V-K7V 211 1
9 V* V406 Vul HXB 18 58 41.580 +22 39 29.40 15.00 15.65 15.31     G5V-K0V 316 0
10 V* QZ Vul HXB 20 02 49.58 +25 14 11.3   19.64 18.2     K3V-K6V 398 0
11 PSR B2145-07.8 Psr 21 45 50.47 -07 50 18.3           ~ 219 0
12 NAME Galactic Bulge reg ~ ~           ~ 3363 0

    Equat.    Gal    SGal    Ecl

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2020.05.28-03:12:40

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