Dawes Review 6: The Impact of Companions on Stellar Evolution

Marco, Orsola De; Izzard, Robert G.

doi:10.1017/pasa.2016.52

Cited by 192 publications

(142 citation statements)

References 420 publications

(630 reference statements)

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“…However, we already know from radial-velocity monitoring that many of the extra-massive thick-disc stars are plausibly multiple systems (Jofré et al 2016). In this work we test the possibility that these stars originate in multiple stellar systems and their properties arise from binary-star interactions (De Marco & Izzard 2017).…”

Section: Introductionmentioning

confidence: 93%

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Binary stars in the Galactic thick disc

Izzard

Preece

Jofré

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The combination of asteroseismologically-measured masses with abundances from detailed analyses of stellar atmospheres challenges our fundamental knowledge of stars and our ability to model them. Ancient red-giant stars in the Galactic thick disc are proving to be most troublesome in this regard. They are older than 5 Gyr, a lifetime corresponding to an initial stellar mass of about 1.2 M . So why do the masses of a sizeable fraction of thick-disc stars exceed 1.3 M , with some as massive as 2.3 M ? We answer this question by considering duplicity in the thick-disc stellar population using a binary population-nucleosynthesis model. We examine how mass transfer and merging affect the stellar mass distribution and surface abundances of carbon and nitrogen. We show that a few per cent of thick-disc stars can interact in binary star systems and become more massive than 1.3 M . Of these stars, most are single because they are merged binaries. Some stars more massive than 1.3 M form in binaries by wind mass transfer. We compare our results to a sample of the APOKASC data set and find reasonable agreement except in the number of these thick-disc stars more massive than 1.3 M . This problem is resolved by the use of a logarithmically-flat orbital-period distribution and a large binary fraction.

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Section: Introductionmentioning

confidence: 93%

“…Lombardi et al 2002;Geller & Mathieu 2011). In binary stars, mass transfer either by direct Roche-lobe overflow or wind mass transfer is relatively common (De Marco & Izzard 2017). The increase in mass of a star causes it to look younger than it actually is (Sandage 1953;Tout et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Binary stars in the Galactic thick disc

Izzard

Preece

Jofré

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The interior structure and evolution (which will only be summarized briefly below) are discussed in the extensive review by Herwig (2005). Nucleosynthesis and stellar yields of single AGB stars are the topic of a recent review by Karakas and Lattanzio (2014), while binary evolution is discussed by De Marco and Izzard (2017). Willson (2000) gives a detailed analysis of problems in deriving a "mass-loss formula", i.e., a quantitative description of how the mass-loss rate depends on fundamental stellar parameters, as used in evolution models.…”

Section: Setting the Stagementioning

confidence: 99%

“…We refer the reader to the recent review by De Marco and Izzard (2017) for a comprehensive overview and an in-depth discussion of the subject. Here, we can only give a flavour of aspects that are being discussed in the AGB literature.…”

Section: Mass Transfer and Binary Evolutionmentioning

confidence: 99%

Mass loss of stars on the asymptotic giant branch

Höfner

Olofsson

2018

Astron Astrophys Rev

469

376

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As low-and intermediate-mass stars reach the asymptotic giant branch (AGB), they have developed into intriguing and complex objects that are major players in the cosmic gas/dust cycle. At this stage, their appearance and evolution are strongly affected by a range of dynamical processes. Large-scale convective flows bring newlyformed chemical elements to the stellar surface and, together with pulsations, they trigger shock waves in the extended stellar atmosphere. There, massive outflows of gas and dust have their origin, which enrich the interstellar medium and, eventually, lead to a transformation of the cool luminous giants into white dwarfs. Dust grains forming in the upper atmospheric layers play a critical role in the wind acceleration process, by scattering and absorbing stellar photons and transferring their outward-directed momentum to the surrounding gas through collisions. Recent progress in high-angularresolution instrumentation, from the visual to the radio regime, is leading to valuable new insights into the complex dynamical atmospheres of AGB stars and their windforming regions. Observations are revealing asymmetries and inhomogeneities in the photospheric and dust-forming layers which vary on time-scales of months, as well as more long-lived large-scale structures in the circumstellar envelopes. High-angularresolution observations indicate at what distances from the stars dust condensation occurs, and they give information on the chemical composition and sizes of dust grains in the close vicinity of cool giants. These are essential constraints for building B Susanne Höfner

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“…However, numerical studies of the CEE that consider only this orbital energy do not manage to eject the common envelope in a persistent and consistent manner (e.g., Taam & Ricker 2010;De Marco et al 2011;Passy et al 2012;Ricker & Taam 2012;Nandez et al 2014; ⋆ E-mail: soker@physics.technion.ac.il Ohlmann et al 2016;Staff et al 2016b;Kuruwita et al 2016;Iaconi et al 2017;De Marco & Izzard 2017;Galaviz et al 2017). These simulations might hint on the need for an extra energy source to eject the envelope.…”

Section: The Grazing Envelope Evolution (Gee)mentioning

confidence: 99%

Grazing envelope evolution towards Type IIb supernovae

Soker¹

2017

Monthly Notices of the Royal Astronomical Society: Letters

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I propose a scenario where the majority of the progenitors of type IIb supernovae (SNe IIb) lose most of their hydrogen-rich envelope during a grazing envelope evolution (GEE). In the GEE the orbital radius of the binary system is about equal to the radius of the giant star, and the more compact companion accretes mass through an accretion disk. The accretion disk is assumed to launch two opposite jets that efficiently remove gas from the envelope along the orbit of the companion. The efficient envelope removal by jets prevents the binary system from entering a common envelope evolution, at least for part of the time. The GEE might be continuous or intermittent. I crudely estimate the total GEE time period to be in the range of about hundreds of years, for a continuous GEE, and up to few tens of thousands of years for intermittent GEE. The key new point is that the removal of envelope gas by jets during the GEE prevents the system from entering a common envelope evolution, and by that substantially increases the volume of the stellar binary parameter space that leads to SNe IIb, both to lower secondary masses and to closer orbital separations.

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Dawes Review 6: The Impact of Companions on Stellar Evolution

Cited by 192 publications

References 420 publications

Binary stars in the Galactic thick disc

Binary stars in the Galactic thick disc

Mass loss of stars on the asymptotic giant branch

Grazing envelope evolution towards Type IIb supernovae

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