2012A&A...543A.121V


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.11CEST14:08:31

2012A&A...543A.121V - Astronomy and Astrophysics, volume 543A, 121-121 (2012/7-1)

Long-term luminosity behavior of 14 ultracompact X-ray binaries.

VAN HAAFTEN L.M., VOSS R. and NELEMANS G.

Abstract (from CDS):

X-ray binaries are usually divided in persistent and transient sources. For ultracompact X-ray binaries (UCXBs), the mass transfer rate is expected to be a strong function of orbital period, predicting persistent sources at short periods and transients at long periods. For 14 UCXBs including two candidates, we investigate the long-term variability and average bolometric luminosity with the purpose of learning how often a source can be expected to be visible above a given luminosity, and we compare the derived luminosities with the theoretical predictions. We use data from the RXTE All-Sky Monitor because of its long-term, unbiased observations. Many UCXBs are faint, i.e., they have a count rate at the noise level for most of the time. Still, information can be extracted from the data, either by using only reliable data points or by combining the bright-end variability behavior with the time-averaged luminosity. Luminosity probability distributions show the fraction of time that a source emits above a given luminosity. All UCXBs show significant variability and relatively similar behavior, though the time-averaged luminosity implies higher variability in systems with an orbital period longer than 40-min. There is no large difference in the statistical luminosity behavior of what we usually call persistent and transient sources. UCXBs with an orbital period below ∼30-min have a time-averaged bolometric luminosity that is in reasonable agreement with estimates based on the theoretical mass transfer rate. Around 40-min the lower bound on the time-averaged luminosity is similar to the luminosity based on the theoretical mass transfer rate, suggesting these sources are indeed faint when not detected. Above 50-min some systems are much brighter than the theoretical mass transfer rate predicts, unless these systems have helium burning donors or lose additional angular momentum.

Abstract Copyright:

Journal keyword(s): X-rays: binaries - binaries: close - stars: neutron - white dwarfs

Simbad objects: 41

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Number of rows : 41

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 ACO 211 ClG 01 32 49 -04 00.6           ~ 16 0
2 4U 0513-40 LXB 05 14 06.59 -40 02 37.0           ~ 155 1
3 NGC 1851 GlC 05 14 06.76 -40 02 47.6   8.80 7.23     ~ 1274 0
4 V* V1055 Ori LXB 06 17 07.3 +09 08 13   18.80 18.5     ~ 522 1
5 4U 0919-54 LXB 09 20 26.4814865475 -55 12 24.507988707 20.40 21.30 21.0     ~ 149 0
6 V* BW Ant LXB 09 29 20.19 -31 23 03.2   18.50 18.63     ~ 177 0
7 4U 1246-58 LXB 12 49 39.364 -59 05 14.68   19.24 18.99     ~ 82 0
8 2E 3049 X 13 26 19.796 -47 29 10.51   26.8   25.3   ~ 19 0
9 NGC 5139 GlC 13 26 47.28 -47 28 46.1   6.12 5.33     ~ 3087 0
10 V* QU TrA LXB 15 47 54.6 -62 34 06           ~ 134 0
11 V* KZ TrA LXB 16 32 16.79 -67 27 39.3 17.40 18.60 18.5     ~ 534 1
12 4U 1705-32 LXB 17 08 54.40 -32 18 57.5           ~ 52 0
13 [KRL2007b] 228 LXB 17 12 35 -37 39.0     12.25     ~ 67 0
14 RX J1718.4-4029 LXB 17 18 24.13 -40 29 30.4           ~ 38 0
15 PSR J1719-14 Psr 17 19 10.073 -14 38 00.96           ~ 51 2
16 [KRL2007b] 238 LXB 17 25 25.50 -32 57 17.5     14.50     ~ 41 0
17 ESO 454-29 GlC 17 27 33.24 -30 48 07.8           ~ 214 0
18 4U 1722-30 LXB 17 27 33.25 -30 48 07.4     12.50     ~ 239 1
19 NAME Slow Burster LXB 17 31 57.73 -33 50 02.5     15.50     ~ 775 1
20 1ES 1735-26.9 LXB 17 38 17.12 -26 59 38.6           ~ 153 0
21 2E 1737.5-2817 LXB 17 40 42.84 -28 18 08.5           ~ 72 0
22 AX J1747.4-3000 LXB 17 47 25.90 -30 00 02.0           ~ 93 0
23 [VVI2000] X2 XB* 17 48 52.43 -20 21 31.7           ~ 11 1
24 NGC 6440 GlC 17 48 52.67 -20 21 34.5   12.01 10.10     ~ 482 1
25 [KRL2007b] 291 LXB 17 51 13.49 -30 37 23.4           ~ 234 0
26 SWIFT J1756.9-2508 LXB 17 56 57.35 -25 06 27.8           ~ 96 0
27 [KRL2007b] 304 LXB 18 06 59.8 -29 24 30           ~ 203 0
28 4U 1812-12 LXB 18 15 06.15 -12 05 46.7           ~ 106 2
29 NGC 6624 GlC 18 23 40.51 -30 21 39.7           ~ 796 1
30 X Sgr X-4 LXB 18 23 40.57 -30 21 40.6   19.06 18.81     ~ 921 1
31 4U 1823-00 LXB 18 25 22.02 -00 00 43.0   23.00 22     ~ 83 0
32 Cl* NGC 6652 SAW V10 LXB 18 35 43.649 -32 59 26.77     18.9     ~ 90 0
33 Cl* NGC 6652 SAW V11 LXB 18 35 44.551 -32 59 38.38         18.72 ~ 11 0
34 NGC 6652 GlC 18 35 45.63 -32 59 26.6   10.64 9.75     ~ 364 0
35 NGC 6712 GlC 18 53 04.32 -08 42 21.5   9.85 8.69     ~ 475 0
36 4U 1850-086 LXB 18 53 04.89 -08 42 19.7 20.40 21.20 21.0     ~ 235 1
37 4U 1857+01 LXB 19 08 26.97 +00 10 07.7 20.50 21.00 20.5     ~ 124 0
38 V* V1405 Aql LXB 19 18 47.871 -05 14 17.09 20.90 21.40 21.0     ~ 446 0
39 CXOU J212958.1+121002 XB* 21 29 58.06 +12 10 02.6     16.6     ~ 65 1
40 4U 2129+12 LXB 21 29 58.3124 +12 10 02.670 14.50 15.70 15.8     ~ 303 1
41 M 15 GlC 21 29 58.33 +12 10 01.2   3       ~ 2950 0

    Equat.    Gal    SGal    Ecl

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2021.04.11-14:08:31

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