The Limiting Stellar Initial Mass for Black Hole Formation in Close Binary Systems

Fryer, Chris L.; Heger, Alexander; Langer, N.; Wellstein, S.

doi:10.1086/342307

Cited by 39 publications

(62 citation statements)

References 32 publications

(40 reference statements)

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“…If binary driven mass loss removes the H-rich mantle in -or shortly after -the main sequence, the He-rich core is exposed for a longer period of time than in single star evolution, allowing the enhanced WR mass loss rates to act for longer. This results in a lower pre-SN core mass and hence the likely formation of a neutron star rather than a black hole (Fryer et al 2002) as appears to be the case in Wd1 (Clark et al 2008;Ritchie et al 2010a). In contrast, a single star will retain its H-rich mantle for longer, be subject to WR mass loss rates for a shorter period of time and will likely yield a Black Hole in the mass range considered here (e.g.…”

Section: Evolutionary Pathways In Wd1mentioning

confidence: 81%

“…Such binary driven mass loss is also predicted to influence the nature of both subsequent supernova (e.g. Paczynski et al 1967;Podsiadlowski et al 1992) and resultant relativistic remnant (Wellstein & Langer 1999;Fryer et al 2002). Moreover, recent evolutionary simulations suggest that in very compact binaries tidal interaction may drive homogeneous chemical evolution permitting the formation of very massive stellar mass black holes ) while it is also suspected that a proportion of Gamma Ray Bursts may result from binary evolution channels (Cantiello et al 2007).…”

Section: Introductionmentioning

confidence: 99%

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A VLT/FLAMES survey for massive binaries in Westerlund 1

Clark

Ritchie

Negueruela

et al. 2011

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Context. There is growing evidence that a treatment of binarity amongst OB stars is essential for a full theory of stellar evolution. However the binary properties of massive stars -frequency, mass ratio & orbital separation -are still poorly constrained. Aims. In order to address this shortcoming we have undertaken a multiepoch spectroscopic study of the stellar population of the young massive cluster Westerlund 1. In this paper we present an investigation into the nature of the dusty Wolf-Rayet star and candidate binary W239. Methods. To accomplish this we have utilised our spectroscopic data in conjunction with multi-year optical and near-IR photometric observations in order to search for binary signatures. Comparison of these data to synthetic non-LTE model atmosphere spectra were used to derive the fundamental properties of the WC9 primary. Results. We found W239 to have an orbital period of only ∼5.05 days, making it one of the most compact WC binaries yet identified. Analysis of the long term near-IR lightcurve reveals a significant flare between 2004-6. We interpret this as evidence for a third massive stellar component in the system in a long period (>6 yr), eccentric orbit, with dust production occuring at periastron leading to the flare. The presence of a near-IR excess characteristic of hot (∼1300 K) dust at every epoch is consistent with the expectation that the subset of persistent dust forming WC stars are short (<1 yr) period binaries, although confirmation will require further observations. Non-LTE model atmosphere analysis of the spectrum reveals the physical properties of the WC9 component to be fully consistent with other Galactic examples. Conclusions. The simultaneous presence of both short period Wolf-Rayet binaries and cool hypergiants within Wd 1 provides compelling evidence for a bifurcation in the post-Main Sequence evolution of massive stars due to binarity. Short period O+OB binaries will evolve directly to the Wolf-Rayet phase, either due to an episode of binary mediated mass loss -likely via case A mass transfer or a contact configuration -or via chemically homogenous evolution. Conversely, long period binaries and single stars will instead undergo a red loop across the HR diagram via a cool hypergiant phase. Future analysis of the full spectroscopic dataset for Wd 1 will constrain the proportion of massive stars experiencing each pathway; hence quantifying the importance of binarity in massive stellar evolution up to and beyond supernova and the resultant production of relativistic remnants.

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Section: Evolutionary Pathways In Wd1mentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Clark

Ritchie

Negueruela

et al. 2011

A&A

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“…The absence of rejuvenation during the case A accretion and the subsequent early exposure of the core results in a sufficiently low pre-SN iron core mass to form a NS rather than a BH (e.g. Fryer et al 2002). We explore this phase of the binary evolution in more detail in Sects.…”

Section: A Pre-sn Binary Evolutionary Pathwaymentioning

confidence: 99%

“…1) suggests that binary driven mass loss resulting in the early onset of WR mass loss rates and hence the production of a low-mass pre-SN core was likewise essential to the formation of a magnetar rather than a BH (cf. Fryer et al 2002). …”

Section: Implications For Magnetar Formationmentioning

confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Clark

Ritchie

Najarro

et al. 2014

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Context. The first soft gamma-ray repeater was discovered over three decades ago, and was subsequently identified as a magnetar, a class of highly magnetised neutron star. It has been hypothesised that these stars power some of the brightest supernovae known, and that they may form the central engines of some long duration gamma-ray bursts. However there is currently no consenus on the formation channel(s) of these objects. Aims. The presence of a magnetar in the starburst cluster Westerlund 1 implies a progenitor with a mass ≥40 M , which favours its formation in a binary that was disrupted at supernova. To test this hypothesis we conducted a search for the putative pre-SN companion.Methods. This was accomplished via a radial velocity survey to identify high-velocity runaways, with subsequent non-LTE model atmosphere analysis of the resultant candidate, Wd1-5. Results. Wd1-5 closely resembles the primaries in the short-period binaries, Wd1-13 and 44, suggesting a similar evolutionary history, although it currently appears single. It is overluminous for its spectroscopic mass and we find evidence of He-and N-enrichement, O-depletion, and critically C-enrichment, a combination of properties that is difficult to explain under single star evolutionary paradigms. We infer a pre-SN history for Wd1-5 which supposes an initial close binary comprising two stars of comparable (∼41 M + 35 M ) masses. Efficient mass transfer from the initially more massive component leads to the mass-gainer evolving more rapidly, initiating luminous blue variable/common envelope evolution. Reverse, wind-driven mass transfer during its subsequent WC Wolf-Rayet phase leads to the carbon pollution of Wd1-5, before a type Ibc supernova disrupts the binary system. Under the assumption of a physical association between Wd1-5 and J1647-45, the secondary is identified as the magnetar progenitor; its common envelope evolutionary phase prevents spin-down of its core prior to SN and the seed magnetic field for the magnetar forms either in this phase or during the earlier episode of mass transfer in which it was spun-up. Conclusions. Our results suggest that binarity is a key ingredient in the formation of at least a subset of magnetars by preventing spin-down via core-coupling and potentially generating a seed magnetic field. The apparent formation of a magnetar in a Type Ibc supernova is consistent with recent suggestions that superluminous Type Ibc supernovae are powered by the rapid spin-down of these objects.

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“…Nevertheless, given the high binary fraction amongst the WR population ) and the need for a low pre-supernova core mass to avoid direct (or fallback) black hole formation (e.g. Fryer et al 2002) it would appear likely that the magnetar progenitor was part of a (now-disrupted) close binary system . Support for this hypothesis comes from population synthesis models, which can only form a neutron star from an isolated ∼60 M progenitor within the ∼5 Myr age of Wd1 if mass loss rates from stellar winds are greatly enhanced (Belczynski & Taam 2008).…”

Section: The Wd1 Magnetarmentioning

confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Ritchie¹,

Clark²,

Negueruela³

et al. 2010

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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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The Limiting Stellar Initial Mass for Black Hole Formation in Close Binary Systems

Cited by 39 publications

References 32 publications

A VLT/FLAMES survey for massive binaries in Westerlund 1

A VLT/FLAMES survey for massive binaries in Westerlund 1

A VLT/FLAMES survey for massive binaries in Westerlund 1

A VLT/FLAMES survey for massive binaries in Westerlund 1

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