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J/A+A/597/A12         LMC X-3 formation history                (Sorensen+, 2017)

Unraveling the formation history of the black hole X-ray binary LMC X-3 from the ZAMS to the present. Sorensen M., Fragos T., Steiner J. F., Antoniou V., Meynet G., Dosopoulou F. <Astron. Astrophys. 597, A12 (2017)> =2017A&A...597A..12S (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Binaries, X-ray Keywords: black hole physics - binaries: general - stars: black holes - stars: evolution - quasars: individual: LMC X-3 - X-stars: binaries Abstract: 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. 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 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. 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≳2.000days) 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 $0.6-1.7days 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=0.8-1.4days. Description: Selected parameters of mass transfer sequence models computed with MESA that matches observational inferred data on the BH X-ray binary LMC X-3. Each record describes the initial configuration of the LMC X-3 binary the moment Roche lobe overflow begins. Objects: ---------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------- 05 38 56.30 -64 05 03.0 LMC X-3 = X LMC X-3 ---------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 77 395 Selected parameters of mass transfer sequences matching LMC X-3
See also: J/A+A/473/523 : Spectroscopic monitoring of 3 neutron stars (Van der Meer+, 2007) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 I4 --- MTseq Mass transfer sequence number 6- 9 F4.2 --- beta Mass transfer efficiency 11- 14 F4.2 Msun MbhRLO Black hole mass at RLO initiation 16- 19 F4.2 Msun M2RLO Donor star mass at RLO initiation 21- 24 F4.2 d PRLO Orbital period at RLO initiation 26- 29 F4.2 --- XcRLO Core fraction of Hydrogen at RLO initiation 31- 35 F5.2 Myr tauRLO Donor star age at RLO initiation 37- 40 F4.2 Msun Mbh Black hole mass at crossing of orbital period 42- 45 F4.2 --- a Black hole spin at crossing of orbital period 47- 50 F4.2 Msun M2 Donor star mass at crossing of orbital period 52- 55 F4.2 [Lsun] logL Donor star Luminosity in log at crossing of orbital period 57- 60 F4.2 --- Xc Core fraction of Hydrogen at crossing of orbital period 62- 66 F5.2 Myr tau Donor star age at crossing of orbital period 68- 72 F5.2 --- p Relative likelihood at crossing of orbital period 74- 77 F4.2 Myr dT Time spent around crossing of orbital period
Acknowledgements: Mads Sorensen, mads.sorensen(at)unige.ch
(End) Mads Sorensen [UNIGE, Suisse], Patricia Vannier [CDS] 03-Oct-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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