Binary Interaction Dominates the Evolution of Massive Stars

Sana, H.; Mink, S. E. de; Koter, A. de; Langer, N.; Evans, C. J.; Gieles, M.; Gosset, Éric; Izzard, Robert G.; Bouquin, J.-B. Le; Schneider, F. R. N.

doi:10.1126/science.1223344

Cited by 1,855 publications

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“…Recent statistics show that among massive stars this frequency can be as high as 70% (de Mink et al 2013), while it climbs to nearly 100% (Sana et al 2012(Sana et al , 2014 for O-type stars. Chini et al (2012) report that the frequency of binaries is higher than 80% for masses M > 16 M , and it steadily decreases to 20% for masses M ∼ 3 M .…”

Section: Effect Carried By the Presence Of A Binary Componentmentioning

confidence: 99%

Critical study of the distribution of rotational velocities of Be stars

Zorec

Frémat

Souza

et al. 2016

A&A

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Context. Among intermediate-mass and massive stars, Be stars are the fastest rotators in the main sequence (MS) and, as such, these stars are a cornerstone to validate models of structure and evolution of rotating stars. Several phenomena, however, induce under-or overestimations either of their apparent Vsin i, or true velocity V. Aims. In the present contribution we aim at obtaining distributions of true rotational velocities corrected for systematic effects induced by the rapid rotation itself, macroturbulent velocities, and binarity. Methods. We study a set of 233 Be stars by assuming they have inclination angles distributed at random. We critically discuss the methods of Cranmer and Lucy-Richardson, which enable us to transform a distribution of projected velocities into another distribution of true rotational velocities, where the gravitational darkening effect on the Vsin i parameter is considered in different ways. We conclude that iterative algorithm by Lucy-Richardson responds at best to the purposes of the present work, but it requires a thorough determination of the stellar fundamental parameters. Results. We conclude that once the mode of ratios of the true velocities of Be stars attains the value V/V c 0.77 in the main-sequence (MS) evolutionary phase, it remains unchanged up to the end of the MS lifespan. The statistical corrections found on the distribution of ratios V/V c for overestimations of Vsin i, due to macroturbulent motions and binarity, produce a shift of this distribution toward lower values of V/V c when Be stars in all MS evolutionary stages are considered together. The mode of the final distribution obtained is at V/V c 0.65. This distribution has a nearly symmetric distribution and shows that the Be phenomenon is characterized by a wide range of true velocity ratios 0.3 V/V c 0.95. It thus suggests that the probability that Be stars are critical rotators is extremely low. Conclusions. The corrections attempted in the present work represent an initial step to infer indications about the nature of the Be-star surface rotation that will be studied in the second paper of this series.

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Section: Effect Carried By the Presence Of A Binary Componentmentioning

confidence: 99%

Critical study of the distribution of rotational velocities of Be stars

Zorec

Frémat

Souza

et al. 2016

A&A

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“…Sana et al 2012). Furthermore, it has been reported recently that the BPASSv2 models are better able to account for (i) the observed shape of the FUV continuum and (ii) UV + optical emission line ratios of star forming galaxies at z ≃ 2 − 3 Strom et al 2016), as well as the properties of massive star clusters in local galaxies (Wofford et al 2016) and Pop III stars (Clark et al 2011;Greif et al 2012;Stacy & Bromm 2013).…”

Section: Methodsologymentioning

confidence: 99%

Effects of binary stellar populations on direct collapse black hole formation

Agarwal

Cullen

Khochfar

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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The critical Lyman-Werner flux required for direct collapse blackholes (DCBH) formation, or J crit , depends on the shape of the irradiating spectral energy distribution (SED). The SEDs employed thus far have been representative of realistic single stellar populations. We study the effect of binary stellar populations on the formation of DCBH, as a result of their contribution to the Lyman-Werner radiation field. Although binary populations with ages > 10 Myr yield a larger LW photon output, we find that the corresponding values of J crit can be up to 100 times higher than single stellar populations. We attribute this to the shape of the binary SEDs as they produce a sub-critical rate of H − photodetaching 0.76 eV photons as compared to single stellar populations, reaffirming the role that H − plays in DCBH formation. This further corroborates the idea that DCBH formation is better understood in terms of a critical region in the H 2 -H − photo-destruction rate parameter space, rather than a single value of LW flux.

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“…Many massive stars are in multiple systems and part of those may follow a different evolution because of interactions with their close companions (Sana et al 2012(Sana et al , 2013. This has triggered many recent works exploring close binary evolution and their consequences for explaining the origin of various stellar populations (see e.g.…”

Section: Multiplicitymentioning

confidence: 99%

Massive stars, successes and challenges

Meynet¹,

Maeder²,

Georgy³

et al. 2016

Proc. IAU

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Abstract. We give a brief overview of where we stand with respect to some old and new questions bearing on how massive stars evolve and end their lifetime. We focus on the following key points that are further discussed by other contributions during this conference: convection, mass losses, rotation, magnetic field and multiplicity. For purpose of clarity, each of these processes are discussed on its own but we have to keep in mind that they are all interacting between them offering a large variety of outputs, some of them still to be discovered.

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Binary Interaction Dominates the Evolution of Massive Stars

Cited by 1,855 publications

References 54 publications

Critical study of the distribution of rotational velocities of Be stars

Critical study of the distribution of rotational velocities of Be stars

Effects of binary stellar populations on direct collapse black hole formation

Massive stars, successes and challenges

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