Formation of high mass X-ray black hole binaries

Brown, G. E.; Heger, Alexander; Langer, N.; Lee, C. H.; Wellstein, S.; Bethe, Hans A.

doi:10.1016/s1384-1076(01)00077-x

Cited by 113 publications

(161 citation statements)

References 35 publications

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“…As has first been argued by Brown et al (1999) and then has been confirmed in detailed calculations by Brown et al (2001), this has to do with differences during helium core burning. Basically the final structure of a star is very different depending on whether the star burns helium with a hydrogen-burning shell around it or without the hydrogen-burning shell (as one would expect if the star loses its envelope before or early during helium burning).…”

Section: Discussionsupporting

confidence: 53%

Models for the Observable System Parameters of Ultraluminous X‐Ray Sources

Madhusudhan

Rappaport

Podsiadlowski

et al. 2008

Astrophysical Journal

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We investigate the evolution of model populations of ultraluminous X-ray sources (ULXs), consisting of a black hole accretor in a binary with a donor star. Two of the models we consider invoke stellar-mass (up to $25 M ) black hole binaries (LMBHs), generated with a binary population synthesis code, while a third model uses intermediatemass ($1000 M ) black hole accretors ( IMBHs). For each model, we computed 30,000 binary evolution sequences. A scheme for calculating the optical flux from ULXs is discussed. We present ''probability images'' for the colormagnitude diagrams (CMDs) and for the orbital periodYX-ray luminosity (P orb -L x ) plane. We show how a population of luminous X-ray sources in a cluster of stars evolves with time. The most probable ULX system parameters correspond to high-mass donors (of initial mass k25 M ) with effective O through late B spectral types, and P orb between 1 and 10 days. Estimates of the numbers of ULXs in a typical galaxy as a function of L x are also presented. We find that if LMBHs are allowed to have super-Eddington L x , the binding energy parameter for the stellar envelope of the black hole progenitor must be k P 0:03 in order not to overproduce ULXs. Comparison of six known ULX counterparts with our model CMDs indicates that the IMBH model somewhat more closely matches the observations. We find that a significant contribution to the optical flux from the IMBH systems comes from intrinsic accretion disk radiation. In effect, IMBH systems, when operating at their maximum luminosities (10 41 Y10 42 ergs s À1 ), are milli-AGNs. While models of IMBH systems during the X-ray phase are attractive, their formation mechanism remains uncertain.

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Section: Discussionsupporting

confidence: 53%

Models for the Observable System Parameters of Ultraluminous X‐Ray Sources

Madhusudhan

Rappaport

Podsiadlowski

et al. 2008

Astrophysical Journal

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“…The main effects, besides from mass loss/gain, are changes in the stellar rotation rate, the nuclear burning scheme and the wind mass-loss rate (de Mink 2010;Langer 2012). As a result, binary interactions affect the final core mass prior to the collapse (Brown et al 2001;Podsiadlowski et al 2004), and therefore possibly the nature of the SN event, the type of compact remnant left behind, the amount of envelope mass ejected, and thus the kinematics of the post-SN binary. Given that almost all massive stars are members of close binaries (Chini et al 2012) and 70 per cent of them interact with their companion star (Sana et al 2012), it is important to probe the evolution leading to SNe in close binaries.…”

Section: Introductionmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

417

613

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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“…In a close binary scenario, however, removal of the hydrogen-rich outer mantle via Case A mass transfer results in a reduced post-MS helium core, and ongoing Case B transfer during shell burning will leave a low mass (≤10 M ) helium-burning WR (P05), permitting isolated neutron star formation within 5 Myr via a type Ib/c supernova if the kick velocity is sufficient to disrupt the system 10 . Neutron star formation may also occur for massive binaries with initial periods greater than a few weeks; such systems will not undergo Roche lobe overflow until core hydrogen burning is complete and therefore form higher-mass helium cores than Case A systems, but if Case B or early-Case C mass transfer can suppress hydrogen shell burning before core helium burning is complete then the consequent reduction in the mass of the iron core may limit black hole formation (Brown et al 2001). Further results on the distribution of binaries on Wd1 from our VLT/FLAMES survey and follow-up observations will therefore allow strong constraints to be placed on the formation channels for such systems.…”

Section: The Wd1 Magnetarmentioning

confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Ritchie¹,

Clark²,

Negueruela³

et al. 2010

A&A

Self Cite

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Context. Westerlund 1 is a young, massive Galactic starburst cluster that contains a rich coeval population of Wolf-Rayet stars, hotand cool-phase transitional supergiants, and a magnetar. Aims. We use spectroscopic and photometric observations of the eclipsing double-lined binary W13 to derive dynamical masses for the two components, in order to determine limits for the progenitor masses of the magnetar CXOU J164710.2-455216 and the population of evolved stars in Wd1. Methods. We use eleven epochs of high-resolution VLT/FLAMES spectroscopy to construct a radial velocity curve for W13. R-band photometry is used to constrain the inclination of the system. Results. W13 has an orbital period of 9.2709 ± 0.0015 days and near-contact configuration. The shallow photometric eclipse rules out an inclination greater than 65 • , leading to lower limits for the masses of the emission-line optical primary and supergiant optical secondary of 21.4 ± 2.6 M and 32.8 ± 4.0 M respectively, rising to 23.2 +3.3 −3.0 M and 35.4 +5.0 −4.6 M for our best-fit inclination 62 +3 −4 degrees. Comparison with theoretical models of Wolf-Rayet binary evolution suggest the emission-line object had an initial mass in excess of ∼35 M , with the most likely model featuring highly non-conservative late-Case A/Case B mass transfer and an initial mass in excess of 40 M . Conclusions. This result confirms the high progenitor mass of the magnetar CXOU J164710.2-455216 inferred from its membership in Wd1, and represents the first dynamical constraint on the progenitor mass of any magnetar. The red supergiants in Wd1 must have similar progenitor masses to W13 and are therefore amongst the most massive stars to undergo a red supergiant phase, representing a challenge for population models that suggest stars in this mass range end their redwards evolution as yellow hypergiants.

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Formation of high mass X-ray black hole binaries

Cited by 113 publications

References 35 publications

Models for the Observable System Parameters of Ultraluminous X‐Ray Sources

Models for the Observable System Parameters of Ultraluminous X‐Ray Sources

Ultra-stripped supernovae: progenitors and fate

A VLT/FLAMES survey for massive binaries in Westerlund 1

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