2012A&A...537A.104V


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET21:25:32

2012A&A...537A.104V - Astronomy and Astrophysics, volume 537A, 104-104 (2012/1-1)

The evolution of ultracompact X-ray binaries.

VAN HAAFTEN L.M., NELEMANS G., VOSS R., WOOD M.A. and KUIJPERS J.

Abstract (from CDS):

Ultracompact X-ray binaries (UCXBs) typically consist of a white dwarf donor and a neutron star or black hole accretor. The evolution of UCXBs and very low mass ratio binaries in general is poorly understood. In particular, the dynamical behavior of an accretion disk extending to a large radius (relative to the orbit) is unclear. We investigate the evolution of UCXBs in order to learn for which mass ratios and accretor types these systems can exist, and if they do, what are their orbital and neutron star spin periods, mass transfer rates and evolutionary timescales. We compute tracks of a binary containing a Roche-lobe overflowing helium white dwarf in which mass transfer is driven by gravitational wave emission. For different assumptions concerning accretion disk behavior we calculate for which system parameters dynamical instability, thermal-viscous disk instability or the propeller effect emerge. The significance of these processes during the evolution of an UCXB is considered. At the onset of mass transfer, the survival of the UCXB is determined by how efficiently the accretor can eject matter in the case of a super-Eddington mass transfer rate. At later times, the evolution of systems strongly depends on the binary's capacity to return angular momentum from the disk to the orbit. We find that this feedback mechanism most likely remains effective even at very low mass ratio. In the case of steady mass transfer, the propeller effect can stop accretion onto recycled neutron stars completely at a sufficiently low mass transfer rate, based on energy considerations. However, mass transfer will likely be non-steady because disk instability allows for accretion of some of the transferred matter. Together, the propeller effect and disk instability cause the low mass ratio UCXBs to be visible a small fraction of the time at most, thereby explaining the lack of observations of such systems. Most likely UCXBs avoid late-time dynamically unstable mass loss from the donor and continue to evolve as the age of the Universe allows. This implies the existence of a large population of low mass ratio binaries with orbital periods ∼70-80min, unless some other mechanism has destroyed these binaries. Even though none have been discovered yet, black hole UCXBs could also exist, at orbital periods of typically 100-110min.

Abstract Copyright:

Journal keyword(s): binaries: close - accretion, accretion disks - X-rays: binaries

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* V1055 Ori LXB 06 17 07.3 +09 08 13   18.80 18.5     ~ 521 1
2 V* BW Ant LXB 09 29 20.19 -31 23 03.2   18.50 18.63     ~ 177 0
3 V* UW CrB LXB 16 05 45.8745535769 +25 51 45.246676152     19.7     ~ 61 0
4 [KRL2007b] 281 LXB 17 48 13.148 -36 07 57.02     20.9     ~ 87 0
5 [VVI2000] X2 XB* 17 48 52.43 -20 21 31.7           ~ 11 1
6 [HAC2010] NGC 6440 X-2 LXB 17 48 52.76 -20 21 24.0           ~ 63 0
7 [KRL2007b] 291 LXB 17 51 13.49 -30 37 23.4           ~ 234 0
8 SWIFT J1756.9-2508 LXB 17 56 57.35 -25 06 27.8           ~ 93 0
9 [KRL2007b] 304 LXB 18 06 59.8 -29 24 30           ~ 203 0
10 V* V4580 Sgr LXB 18 08 27.54 -36 58 44.3   16.81 16.51     ~ 890 0
11 V* V4634 Sgr LXB 18 29 28.2 -23 47 49 18.90 19.40 19     ~ 298 0
12 2MAXI J1900-248 LXB 19 00 08.65 -24 55 13.7     18.09     ~ 186 0
13 PSR B1937+21 Psr 19 39 39.6 +21 37 22           ~ 975 2
14 NGC 7009 PN 21 04 10.8153350719 -11 21 48.581808296   12.48 12.07     ~ 969 1
15 V* SS Cyg DN* 21 42 42.8034554117 +43 35 09.863763484 11.07 8.2 7.70     K5V 1222 1
16 NAME Galactic Bulge reg ~ ~           ~ 3531 0

    Equat.    Gal    SGal    Ecl

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2021.03.01-21:25:32

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