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 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:
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RA (2000) DE Designation(s)
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05 38 56.30 -64 05 03.0 LMC X-3 = X LMC X-3
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 77 395 Selected parameters of mass transfer sequences
matching LMC X-3
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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
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Bytes Format Units Label Explanations
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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
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Acknowledgements:
Mads Sorensen, mads.sorensen(at)unige.ch
(End) Mads Sorensen [UNIGE, Suisse], Patricia Vannier [CDS] 03-Oct-2016