Evolution of Very Massive Stars.

Schwarzschild, M.; Härm, R.

doi:10.1086/146548

Cited by 174 publications

(113 citation statements)

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“…This code adopts the opacities from Iglesias et al (1992) and the nuclear reaction rates from Fowler et al (1975). Semi-convection is treated according to the criterion of Schwarzschild & Harm (1958) and convective core overshooting is included as in Schaller et al (1992). The formalisms used to calculate the effect on evolution of stellar wind mass loss rates deserve some special attention.…”

Section: Massive Single Star Evolutionmentioning

confidence: 99%

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

Mennekens

Vanbeveren

2014

A&A

173

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 Single Star Evolutionmentioning

confidence: 99%

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

Mennekens

Vanbeveren

2014

A&A

173

197

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“…This is the difficulty met by Schwarzschild & Härm (1958) when they studied the evolution of massive main sequence stars where electron scattering is the main source of opacity. This led them to introduce semi-convection into models of these stars.…”

Section: The Chemical Composition Is Discontinuous But There Is No Momentioning

confidence: 99%

Proper use of Schwarzschild Ledoux criteria in stellar evolution computations

Gabriel

Noels

Montalbán

et al. 2014

A&A

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The era of detailed asteroseismic analyses opened by space missions such as CoRoT and Kepler has highlighted the need for stellar models devoid of numerical inaccuracies, in order to be able to diagnose which physical aspects are being ignored or poorly treated in standard stellar modeling. We tackle here the important problem of fixing convective zone boundaries in the frame of the local mixing length theory. First we show that the only correct way to locate a convective zone boundary is to find, at each iteration step, through interpolations or extrapolations from points within the convective zone, the mass where the radiative luminosity is equal to the total luminosity. We then discuss two misuses of the boundary condition and the ways they affect stellar modeling and stellar evolution. The first consists in applying the neutrality condition for convective instability on the radiative side of the convective boundary. The second way of misusing the boundary condition comes from the process of fixing the convective boundary through the search for a change of sign of a possibly discontinuous function. We show that these misuses can lead to completely wrong estimates of convective core sizes with important consequences for the following evolutionary phases. We point out the advantages of using a double mesh point at each convective zone boundary. The specific problem of a convective shell is discussed and some remarks concerning overshooting are given.

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“…The convective zone boundaries are defined either with the Schwarzschild criterion (Schwarzschild and Härm 1958) or the Ledoux criterion (Ledoux 1947). For the latter case, the Ledoux temperature gradient is defined as…”

Section: Mixing Prescriptionsmentioning

confidence: 99%

“…Opacities are increased outside the core by electron scattering, where a chemical discontinuity appears as a result of this core expansion. Since the pioneer work of Schwarzschild and Härm (1958), several authors have investigated the occurrence of semiconvective mixing in massive stars and its effects on stellar evolution (see, e.g., Stothers 1970;Stothers and Chin 1975;Langer 1985).…”

Section: Introductionmentioning

confidence: 99%

Semiconvective mixing in low-mass stars

Aguirre

Ballot

Serenelli

et al. 2010

Astrophys Space Sci

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Mixing processes such as convection, overshooting and rotational mixing have long been known to affect the evolutionary properties of low-mass stars. While modeling a 1.2 M star, we encountered a semiconvective region outside the fully convective core, reminiscent of the wellknown situation for massive stars. In this study we focus on low-mass stars presenting convective cores and, by applying different prescriptions for the determination of the convective boundaries and, using different mixing descriptions for the dynamical processes in the core, we look for the effects of semiconvective mixing in the interior structure of the stars and its observable quantities. With this purpose, we have constructed different sets of evolutionary models using a stellar evolution code (GARSTEC), and analyzed the models looking for imprints of these processes.

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Evolution of Very Massive Stars.

Cited by 174 publications

References 0 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

Proper use of Schwarzschild Ledoux criteria in stellar evolution computations

Semiconvective mixing in low-mass stars

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