Magnetic massive stars as progenitors of ‘heavy’ stellar-mass black holes

Petit, Véronique; Keszthelyi, Z.; Macinnis, R.; Cohen, David H.; Townsend, R. H. D.; Wade, G. A.; Thomas, SMITH; Owocki, S. P.; Puls, J.; ud‐Doula, Asif

doi:10.1093/mnras/stw3126

Cited by 107 publications

(133 citation statements)

References 81 publications

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“…Low-metallicity progenitors are believed to have weaker stellar winds and hence diminished mass loss [112]. Given the mass of the primary black hole, the progenitors of GW170104 likely formed in a lower metallicity environment Z ≲ 0.5Z ⊙ [6,100,[113][114][115], but low mass loss may also have been possible at higher metallicity if the stars were strongly magnetized [116].…”

Section: Astrophysical Implicationsmentioning

confidence: 99%

GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

2,319

1,861

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We describe the observation of GW170104, a gravitational-wave signal produced by the coalescence of a pair of stellar-mass black holes. The signal was measured on January 4, 2017 at 10∶11:58.6 UTC by the twin advanced detectors of the Laser Interferometer Gravitational-Wave Observatory during their second observing run, with a network signal-to-noise ratio of 13 and a false alarm rate less than 1 in 70 000 years. −0.07 . We constrain the magnitude of modifications to the gravitational-wave dispersion relation and perform null tests of general relativity. Assuming that gravitons are dispersed in vacuum like massive particles, we bound the graviton mass to m g ≤ 7.7 × 10 −23 eV=c 2 . In all cases, we find that GW170104 is consistent with general relativity.

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Section: Astrophysical Implicationsmentioning

confidence: 99%

GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

2,319

1,861

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“…However, other uncertainties (with possible degeneracies) are known, for example in the treatment of rotation, magnetic fields (e.g., Petit et al 2017), convective mixing, and overshooting (e.g., Arnett et al 2015;Arnett 2015;Arnett & Meakin 2016;3 These are available at https://stellarcollapse.org/ renzo2017 Farmer et al 2016). The coupling of these uncertainties with the wind mass loss may modify the outcomes of our numerical experiments.…”

Section: Discussionmentioning

confidence: 99%

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

Renzo¹,

Ott²,

Shore³

et al. 2017

A&A

136

150

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Mass loss processes are a key uncertainty in the evolution of massive stars. They determine the amount of mass and angular momentum retained by the star, thus influencing its evolution and presupernova structure. Because of the high complexity of the physical processes driving mass loss, stellar evolution calculations must employ parametric algorithms, and usually only include wind mass loss. We carried out an extensive parameter study of wind mass loss and its effects on massive star evolution using the open-source stellar evolution code MESA. We provide a systematic comparison of wind mass loss algorithms for solar-metallicity, nonrotating, single stars in the initial mass range of 15 M to 35 M . We consider combinations drawn from two hot phase (i.e., roughly the main sequence) algorithms, three cool phase (i.e., post-main-sequence) algorithms, and two Wolf-Rayet mass loss algorithms. We discuss separately the effects of mass loss in each of these phases. In addition, we consider linear wind efficiency scale factors of 1, 0.33, and 0.1 to account for suggested reductions in mass loss rates due to wind inhomogeneities. We find that the initial to final mass mapping for each zero-age main-sequence (ZAMS) mass has a ∼50% uncertainty if all algorithm combinations and wind efficiencies are considered. The ad-hoc efficiency scale factor dominates this uncertainty. While the final total mass and internal structure of our models vary tremendously with mass loss treatment, final luminosity and effective temperature are much less sensitive for stars with ZAMS mass 30 M . This indicates that uncertainty in wind mass loss does not negatively affect estimates of the ZAMS mass of most single-star supernova progenitors from pre-explosion observations. Our results furthermore show that the internal structure of presupernova stars is sensitive to variations in both main sequence and post main-sequence mass loss. The compactness parameter ξ ∝ M/R(M) has been identified as a proxy for the "explodability" of a given presupernova model. We find that ξ varies by as much as 30% for models of the same ZAMS mass evolved with different wind efficiencies and mass loss algorithm combinations. This suggests that the details of the mass loss treatment might bias the outcome of detailed core-collapse supernova calculations and the predictions for neutron star and black hole formation.

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“…These effects are based on the dynamical interactions between the magnetosphere and the stellar wind, and we conclude from our model calculations that they have a large impact on massive star evolution. Two evolutionary scenarios are discussed by Petit et al (2017) and Georgy et al (in press). Petit et al (2013) and Shultz et al (in prep).…”

Section: Discussionmentioning

confidence: 99%

The evolution of magnetic hot massive stars: Implementation of the quantitative influence of surface magnetic fields in modern models of stellar evolution

2016

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Abstract.Large-scale dipolar surface magnetic fields have been detected in a fraction of OB stars, however only few stellar evolution models of massive stars have considered the impact of these fossil fields. We are performing 1D hydrodynamical model calculations taking into account evolutionary consequences of the magnetospheric-wind interactions in a simplified parametric way. Two effects are considered: i) the global mass-loss rates are reduced due to mass-loss quenching, and ii) the surface angular momentum loss is enhanced due to magnetic braking. As a result of the magnetic mass-loss quenching, the mass of magnetic massive stars remains close to their initial masses. Thus magnetic massive stars -even at Galactic metallicity -have the potential to be progenitors of 'heavy' stellar mass black holes. Similarly, at Galactic metallicity, the formation of pair instability supernovae is plausible with a magnetic progenitor.

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Magnetic massive stars as progenitors of ‘heavy’ stellar-mass black holes

Cited by 107 publications

References 81 publications

GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2

GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

The evolution of magnetic hot massive stars: Implementation of the quantitative influence of surface magnetic fields in modern models of stellar evolution

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