2017A&A...597A..12S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST11:43:44

2017A&A...597A..12S - Astronomy and Astrophysics, volume 597A, 12-12 (2017/1-1)

Unraveling the formation history of the black hole X-ray binary LMC X-3 from the zero age main sequence to the present.

SORENSEN M., FRAGOS T., STEINER J.F., ANTONIOU V., MEYNET G. and DOSOPOULOU F.

Abstract (from CDS):

Aims. We have endeavoured to understand the formation and evolution of the black hole (BH) X-ray binary LMC X-3. We estimated the properties of the system at four evolutionary stages: (1) at the zero-age main-sequence (ZAMS); (2) immediately before the supernova (SN) explosion of the primary; (3) immediately after the SN; and (4) at the moment when Roche-lobe overflow began.
Methods. We used a hybrid approach that combined detailed calculations of the stellar structure and binary evolution with approximate population synthesis models. This allowed us to estimate potential natal kicks and the evolution of the BH spin. We incorporated as model constraints the most up-to-date observational information throughout, which include the binary orbital properties, the companion star mass, effective temperature, surface gravity and radius, and the BH mass and spin.
Results. We find at 5% and 95% confidence, respectively, that LMC X-3 began as a ZAMS system with the mass of the primary star in the range M1,ZAMS=22-31M and a secondary star of M2,ZAMS=5.0-8.3M, in a wide (PZAMS≥2.000-days) and eccentric (eZAMS≥0.18) orbit. Immediately before the SN, the primary had a mass of M1,preSN=11.1-18.0M, but the secondary star was largely unaffected. The orbital period decreased to 0.6-1.7-days and is still eccentric 0≤epreSN≤0.44. We find that a symmetric SN explosion with no or small natal kicks (a few tens of km/s) imparted on the BH cannot be formally excluded, but large natal kicks in excess of ≥120km/s increase the estimated formation rate by an order of magnitude. Following the SN, the system has a BH MBH,postSN=6.4-8.2M and is set on an eccentric orbit. At the onset of the Roche-lobe overflow, the orbit is circular and has a period of PRLO=0.8-1.4-days.

Abstract Copyright: © ESO, 2016

Journal keyword(s): black hole physics - binaries: general - stars: black holes - stars: evolution - quasars: individual: LMC X-3 - X-rays: binaries

VizieR on-line data: <Available at CDS (J/A+A/597/A12): table2.dat>

Simbad objects: 13

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Number of rows : 13

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           ~ 148 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9446 1
3 NAME M33 X-7 HXB 01 33 34.13 +30 32 11.3 17.50 18.80 18.70     O 127 2
4 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
5 X LMC X-2 LXB 05 20 28.04 -71 57 53.3 17.20 18.00 18.0     ~ 169 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
7 X LMC X-3 HXB 05 38 56.6325045489 -64 05 03.321118015   17 17.2     B2.5Ve 630 0
8 X LMC X-1 HXB 05 39 38.8285930597 -69 44 35.533031148   14.8 14.5     O8(f)p 560 2
9 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 721 0
10 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1701 1
11 Granat 1915+105 LXB 19 15 11.54938 +10 56 44.7585           ~ 2284 0
12 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3924 0
13 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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2020.07.10-11:43:44

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