The VLT-FLAMES survey of massive stars: NGC 346-013 as a test case for massive close binary evolution

Massive stars with a core-halo structure are interesting objects for stellar physics and hydrodynamics. Using simulations for stellar evolution, radiation hydrodynamics, and radiative transfer, we study the explosion of stars with an extended and tenuous envelope (i.e. stars in which 95% of the mass is contained within 10% or less of the surface radius). We consider both H-rich supergiant and He-giant progenitors resulting from close-binary evolution and dying with a final mass of 2.8–5 M⊙. An extended envelope causes the supernova (SN) shock to brake and a reverse shock to form, sweeping core material into a dense shell. The shock-deposited energy, which suffers little degradation from expansion, is trapped in ejecta layers of moderate optical depth, thereby enhancing the SN luminosity at early times. With the delayed 56Ni heating, we find that the resulting optical and near-IR light curves all exhibit a double-peak morphology. We show how an extended progenitor can explain the blue and featureless optical spectra of some Type IIb and Ib SNe. The dense shell formed by the reverse shock leads to line profiles with a smaller and near-constant width. This ejecta property can explain the statistically narrower profiles of Type IIb compared to Type Ib SNe, as well as the peculiar Hα profile seen in SN 1993J. At early times, our He-giant star explosion model shows a high luminosity, a blue colour, and featureless spectra reminiscent of the Type Ib SN 2008D, suggesting a low-mass progenitor.

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New massive close binary models and the26Al yield of the WR component of γ VEL

Symposium - International Astronomical Union ◽

10.1017/s0074180900202179 ◽

1995 ◽

Vol 163 ◽

pp. 305-308 ◽

Cited By ~ 1

Author(s):

H. Braun ◽

N. Langer

Keyword(s):

Milky Way ◽

Binary Code ◽

Chemical Species ◽

Time Dependent ◽

Close Binary ◽

Reaction Networks ◽

Γ Ray ◽

Binary Evolution ◽

First Time ◽

Massive Close Binary

We present new models of massive close binary evolution, using an up-to-date hydrodynamic binary code which includes time dependent mixing of chemical species in the stellar interior, and nuclear reaction networks for the CNO cycles as well as for the NeNa and MgAl cycles. Some of our models, tailored to fit γ Vel, provide for the first time detailed results for the production and ejection of26A1 into the interstellar medium by WR binaries. From our results one can estimate the contribution of WR stars to the amount of26Al presently seen in the Milky Way by γ-ray satellites.

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Rotation and Massive Close Binary Evolution

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308020462 ◽

2007 ◽

Vol 3 (S250) ◽

pp. 167-178 ◽

Cited By ~ 8

Author(s):

Norbert Langer ◽

Matteo Cantiello ◽

Sung-Chul Yoon ◽

Ian Hunter ◽

Ines Brott ◽

...

Keyword(s):

Binary Systems ◽

Close Binary ◽

Single Star ◽

Essential Ingredient ◽

Critical Rotation ◽

Close Binary Systems ◽

Star Models ◽

Binary Evolution ◽

Massive Close Binary

AbstractWe review the role of rotation in massive close binary systems. Rotation has been advocated as an essential ingredient in massive single star models. However, rotation clearly is most important in massive binaries where one star accretes matter from a close companion, as the resulting spin-up drives the accretor towards critical rotation. Here, we explore our understanding of this process, and its observable consequences. When accounting for these consequences, the question remains whether rotational effects in massive single stars are still needed to explain the observations.

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The influence of close binary evolution on the distribution of massive stars in the HR diagram

Astrophysics and Space Science ◽

10.1007/bf00640460 ◽

1988 ◽

Vol 149 (1) ◽

pp. 1-12 ◽

Cited By ~ 5

Author(s):

D. Vanbeveren

Keyword(s):

Massive Stars ◽

Close Binary ◽

Binary Evolution ◽

Hr Diagram

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Population Synthesis of Massive Close Binary Evolution

Handbook of Supernovae ◽

10.1007/978-3-319-21846-5_125 ◽

2017 ◽

pp. 671-692

Author(s):

J. J. Eldridge

Keyword(s):

Close Binary ◽

Population Synthesis ◽

Binary Evolution ◽

Massive Close Binary

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Structure and evolution of massive single stars and their relevance for close binary systems

Symposium - International Astronomical Union ◽

10.1017/s0074180900201514 ◽

1995 ◽

Vol 163 ◽

pp. 15-23

Author(s):

Norbert Langer

Keyword(s):

Binary Systems ◽

Massive Stars ◽

Close Binary ◽

Single Star ◽

Close Binary Systems ◽

Massive Close Binary

Differences in the evolution of massive single stars and components of massive close binary systems are investigated. While for stars above the red supergiant luminosity limit, single star and case B primary evolution merge into a single scenario, large differences for less massive stars are demonstrated to occur at the example of MZAMS = 40M⊙, concerning the various WR subtypes, the nucleosynthesis yields, and the supernova stage.

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The evolution of massive binary systems

Serbian Astronomical Journal ◽

10.2298/saj2001001p ◽

2020 ◽

pp. 1-13

Author(s):

Jelena Petrovic

Keyword(s):

Binary Systems ◽

Gamma Ray ◽

Massive Stars ◽

Compact Objects ◽

Close Binary ◽

Extensive Literature ◽

Single Star ◽

Close Binary Systems ◽

Massive Binary Systems ◽

Massive Close Binary

The evolution of massive stars in close binary systems is significantly different from single star evolution due to a series of interactions between the two stellar components. Such massive close binary systems are linked to various astrophysical phenomena, for example Wolf-Rayet stars, supernova type Ib and Ic, X-ray binaries and gamma-ray bursts. Also, the emission of gravitational waves, recently observed by the LIGO-Virgo detectors, is associated with mergers in binary systems containing compact objects, relics of massive stars - black holes and neutron stars. Evolutionary calculations of massive close binary systems were performed by various authors, but many aspects are not yet fully understood. In this paper, the main concepts of massive close binary evolution are reviewed, together with the most important parameters that can influence the final outcome of the binary system evolution, such as rotation, magnetic fields, stellar wind mass loss and mass accretion efficiency during interactions. An extensive literature overview of massive close binary models in the light of exciting observations connected with those systems is presented.

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Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936528 ◽

2020 ◽

Vol 636 ◽

pp. A104 ◽

Cited By ~ 43

Author(s):

K. Belczynski ◽

J. Klencki ◽

C. E. Fields ◽

A. Olejak ◽

E. Berti ◽

...

Keyword(s):

Black Hole ◽

Angular Momentum ◽

Massive Stars ◽

Momentum Transport ◽

High Mass ◽

Close Binary ◽

Angular Momentum Transport ◽

Efficient Transport ◽

Binary Evolution ◽

Merger Rate

All ten LIGO/Virgo binary black hole (BH-BH) coalescences reported following the O1/O2 runs have near-zero effective spins. There are only three potential explanations for this. If the BH spin magnitudes are large, then: (i) either both BH spin vectors must be nearly in the orbital plane or (ii) the spin angular momenta of the BHs must be oppositely directed and similar in magnitude. Then there is also the possibility that (iii) the BH spin magnitudes are small. We consider the third hypothesis within the framework of the classical isolated binary evolution scenario of the BH-BH merger formation. We test three models of angular momentum transport in massive stars: a mildly efficient transport by meridional currents (as employed in the Geneva code), an efficient transport by the Tayler-Spruit magnetic dynamo (as implemented in the MESA code), and a very-efficient transport (as proposed by Fuller et al.) to calculate natal BH spins. We allow for binary evolution to increase the BH spins through accretion and account for the potential spin-up of stars through tidal interactions. Additionally, we update the calculations of the stellar-origin BH masses, including revisions to the history of star formation and to the chemical evolution across cosmic time. We find that we can simultaneously match the observed BH-BH merger rate density and BH masses and BH-BH effective spins. Models with efficient angular momentum transport are favored. The updated stellar-mass weighted gas-phase metallicity evolution now used in our models appears to be key for obtaining an improved reproduction of the LIGO/Virgo merger rate estimate. Mass losses during the pair-instability pulsation supernova phase are likely to be overestimated if the merger GW170729 hosts a BH more massive than 50 M⊙. We also estimate rates of black hole-neutron star (BH-NS) mergers from recent LIGO/Virgo observations. If, in fact. angular momentum transport in massive stars is efficient, then any (electromagnetic or gravitational wave) observation of a rapidly spinning BH would indicate either a very effective tidal spin up of the progenitor star (homogeneous evolution, high-mass X-ray binary formation through case A mass transfer, or a spin- up of a Wolf-Rayet star in a close binary by a close companion), significant mass accretion by the hole, or a BH formation through the merger of two or more BHs (in a dense stellar cluster).

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