The stability of massive main-sequence stars as a function of metallicity

Shiode, J.; Quataert, Eliot; Arras, Phil

doi:10.1111/j.1365-2966.2012.21130.x

Cited by 16 publications

(12 citation statements)

References 27 publications

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“…On the other hand, masses of Population III stars could be much higher due to the absence of effective coolants in the primordial gas. Then, their masses could be limited by pulsations, though, the upper mass limit remains undefined [703] and masses up to ≃ 1000 M ⊙ are often inferred in theoretical studies.…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

462

382

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We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

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Section: Introductionmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

462

382

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“…In Figure 7, we show the linear frequency, the coupling coefficient with the parent mode (Weinberg et al 2012), and the linear damping rate due to turbulent convection of each daughter mode (Shiode et al 2012;Burkart et al 2013).…”

Section: B Tidal Angular Momentum Transfermentioning

confidence: 99%

Tidal evolution and diffusive growth during high-eccentricity planet migration: revisiting the eccentricity distribution of hot Jupiters

Yu,

Weinberg,

Arras

2021

Preprint

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High-eccentricity tidal migration is a potential formation channel for hot Jupiters. During this process, the planetary f-mode may experience a phase of diffusive growth, allowing its energy to quickly build up to large values. In Yu et al. ( 2021), we demonstrated that nonlinear mode interactions between a parent f-mode and daughter f-and p-modes expand the parameter space over which the diffusive growth of the parent is triggered. We extend that study by incorporating (1) the angular momentum transfer between the orbit and the mode, and consequently the evolution of the pericenter distance, (2) a phenomenological correction to the nonlinear frequency shift at high parent mode energies, and (3) dissipation of the parent's energy due to both turbulent convective damping of the daughter modes and strongly nonlinear wave-breaking events. The new ingredients allow us to follow the coupled evolution of the mode and orbit over 10 4 years, covering the diffusive evolution from its onset to its termination. We find that the semi-major axis shrinks by a factor of nearly ten over 10 4 years, corresponding to a tidal quality factor Q ∼ 10. The f-mode's diffusive growth terminates while the eccentricity is still high, at around e = 0.8 − 0.95. Using these results, we revisit the eccentricity distribution of proto-hot Jupiters. We estimate that less than 1 proto-HJ with eccentricity > 0.9 should be expected in Kepler 's data once the diffusive regime is accounted for, explaining the observed paucity of this population.

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“…We select four pairs of models with similar reference core masses of M ref He core 4.3, 5.4, 5.7, 6.3 M . 4 Assuming no dynamical transient happen shortly before corecollapse (e.g., Shiode et al 2012;Khazov et al 2016;Fuller 2017;Fuller & Ro 2018) We focus on the composition inside the helium core. The radius of each diagram is proportional to the total helium core mass.…”

Section: Composition At Core Collapsementioning

confidence: 99%

Different to the core: the pre-supernova structures of massive single and binary-stripped stars

Laplace,

Justham,

Renzo

et al. 2021

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The majority of massive stars live in binary or multiple systems and will interact during their lifetimes, which helps to explain the observed diversity of core-collapse supernovae. Donor stars in binary systems can lose most of their hydrogen-rich envelopes through mass transfer. As a result, not only are the surface properties affected, but also the core structure. However, most calculations of the core-collapse properties of massive stars rely on single-star models. We present a systematic study of the difference between the pre-supernova structures of single stars and stars of the same initial mass (11 -21 M ) that have been stripped due to stable post-main sequence mass transfer at solar metallicity. We present the pre-supernova core composition with novel diagrams that give an intuitive representation of the isotope distribution. As shown in previous studies, at the edge of the carbon-oxygen core, the binary-stripped star models contain an extended gradient of carbon, oxygen, and neon. This layer remains until core collapse and is more extended in mass for higher initial stellar masses. It originates from the receding of the convective helium core during core helium burning in binary-stripped stars, which does not occur in single-star models. We find that this same evolutionary phase leads to systematic differences in the final density and nuclear energy generation profiles. Binary-stripped star models have systematically higher total masses of carbon at the moment of core collapse compared to single star models, which likely results in systematically different supernova yields. In about half of our models, the silicon-burning and oxygen-rich layers merge after core silicon burning. We discuss the implications of our findings for the explodability, supernova observations, and nucleosynthesis from these stars. Our models will be publicly available and can be readily used as input for detailed supernova simulations.

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The stability of massive main-sequence stars as a function of metallicity

Cited by 16 publications

References 27 publications

The Evolution of Compact Binary Star Systems

The Evolution of Compact Binary Star Systems

Tidal evolution and diffusive growth during high-eccentricity planet migration: revisiting the eccentricity distribution of hot Jupiters

Different to the core: the pre-supernova structures of massive single and binary-stripped stars

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