The Zero-Age Main Sequence

Kippenhahn, Rudolf; Weigert, Alfred; Weiß, Achim

doi:10.1007/978-3-642-30304-3_22

Cited by 112 publications

(143 citation statements)

References 3 publications

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“…2.1 also applies here. Following the classification of Kippenhahn & Weigert (1967) and Lauterborn (1970), we distinguish three main phases of RLOF, which correspond to the three major expansion phases during stellar evolution: case A where the RLOF takes place during the core hydrogen burning phase of the mass loser, case B where the RLOF occurs during the hydrogen shell burning phase prior to the blue loop phase during central helium burning (see also Schaller et al 1992), and case C where the RLOF begins after helium has been depleted in the core. Case B RLOF is additionally divided into early case B or case Br, where at the onset of RLOF the envelope of the mass loser is mostly radiative, and late case B or case Bc, where the primary has a deep convective envelope at the beginning of the RLOF phase.…”

Section: Massive Close Binary Evolutionmentioning

confidence: 99%

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Mennekens

Vanbeveren

2014

A&A

172

197

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With our galactic evolutionary code that contains a detailed intermediate-mass and massive binary population model, we study the temporal evolution of the galactic population of double neutron star binaries, mixed systems with a neutron star and black hole component, and double black hole binaries. We computed the merger rates of these relativistic binaries and translate them into LIGO II detection rates. We demonstrate that accounting for the uncertainties in the relation "initial mass-final mass" predicted by massive close binary evolution and due to the possible effect of large stellar wind mass loss during the luminous blue variable phase of a star with initial mass higher than 30−40 M and during the red supergiant phase of a star with initial mass lower than 30−40 M when such a star is a binary component, the double black hole merger rate may be very low, contrary to predictions made by other groups. Hydrodynamic computations of the r-process chemical yields ejected during the relativistic binary merger process have recently become available. With our galactic code that includes binaries, it is then straightforward to calculate the temporal galactic evolution of the r-process elements ejected by these mergers. We conclude that except for the earliest evolutionary phase of the Galaxy (∼the first 100 Myr), double compact star mergers may be the major production sites of r-process elements, and it is probable that the mixed systems dominate this production over double neutron star binary mergers.

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Section: Massive Close Binary Evolutionmentioning

confidence: 99%

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Mennekens

Vanbeveren

2014

A&A

172

197

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“…According to the canonical criterion for mass-transfer (Kippenhahn & Weigert 1967) one simply has to ask whether the donor star radius, R 2 is larger or smaller than its Roche-lobe The meaning of the various symbols is equivalent to those in Fig. 3.…”

Section: Break-down Of the Applied Mass-transfer Scheme For Giant Donorsmentioning

confidence: 99%

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris

Sanyal

Yoon

et al. 2013

A&A

141

181

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Context. Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Aims. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Methods. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre-and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD (treated as a point mass) in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. Results. We show that recycled pulsars may form via AIC from all three types of progenitor systems investigated and find that the final properties of the resulting MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, as a consequence of the fine-tuned mass-transfer rate necessary to make the WD grow in mass, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. In addition, their predicted small space velocities can also be used to identify them observationally. The production time of NSs formed via AIC can exceed 10 Gyr which can therefore explain the existence of relatively young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions.

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“…Following Kippenhahn & Weigert (1967), case B mass transfer starts once the more massive star has left its main sequence and crosses the Hertzsprung gap. Similarly to case A, it proceeds in two steps: a rapid phase during which the mass loss rate rises up to about 10 −4 M yr −1 and the mass ratio is reversed, followed by a slow phase during which little mass is accreted but most of the orbital changes take place.…”

Section: Case B Mass Transfermentioning

confidence: 99%

BINSTAR: a new binary stellar evolution code

Siess

Izzard

Davis

et al. 2013

A&A

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We provide a detailed description of a new stellar evolution code, BINSTAR, which has been developed to study interacting binaries. Based on the stellar evolution code STAREVOL, it is specifically designed to study low-and intermediate-mass binaries. We describe the state-of-the-art input physics, which includes treatments of tidal interactions, mass transfer and angular momentum exchange within the system. A generalised Henyey method is used to solve simultaneously the stellar structure equations of each component as well as the separation and eccentricity of the orbit. Test simulations for cases A and B mass transfer are presented and compared with available models. The results of the evolution of Algol systems are in remarkable agreement with the calculations of the Vrije Universiteit Brussel (VUB) group, thus validating our code. We also computed a large grid of models for various masses (2 ≤ M/M ≤ 20) and seven metallicities (Z = 0.0001, 0.001, 0.004, 0.008, 0.01, 0.02, 0.03) to provide a useful analytical parameterisation of the tidal torque constant E 2 , which allows the determination of the circularisation and synchronisation timescales for stars with a radiative envelope and convective core. The evolution of E 2 during the main sequence shows noticeable differences compared to available models. In particular, our new calculations indicate that the circularisation timescale is constant during core hydrogen burning. We also show that E 2 weakly depends on core overshooting but is substantially increased when the metallicity becomes lower.

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The Zero-Age Main Sequence

Cited by 112 publications

References 3 publications

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

BINSTAR: a new binary stellar evolution code

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