On the Maximum Mass of Stable Stars.

Schwarzschild, M.; Härm, R.

doi:10.1086/146662

Cited by 115 publications

(43 citation statements)

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“…Ledoux [6] demonstrated the existence of a critical mass below which stars are pulsationally stable against adiabatic oscillations on the main sequence. For normal stars containing about 2% of heavy elements, Schwarzschild and Härm [7] established this mass limit around 60 M ⊙ .…”

Section: Introductionmentioning

confidence: 89%

Structure and stability of primordial stars

Karafistan¹

2016

Turk J Phys

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Abstract:For decades large-scale cosmic structures have been modeled as the gravitational amplification of small-density perturbations of the cosmological recombination epoch of the Big Bang. In astrophysics, cosmological nucleosynthesis is considered responsible for the production of the pristine gas, which should be found in the first-generation stars in the form of hydrogen and helium as the main constituents. In the later type of second-generation stars, hydrogen is converted into helium by the CN-cycle reactions, in which heavier elements are produced. These elements are believed to enrich the intergalactic medium by possible star bursts at the last stages of evolution.Stability criteria in the stellar evolutionary models pointed out that first-generation stars should be massive and live long enough for the nucleosynthesis of the natural elements, heavier than hydrogen and helium. Initially, they were expected to be very faint and blue to be observed spectroscopically. Nowadays, more and more metal-deficient star observations, made possible by the new era of space telescopes, are interpreted as the discovery of a primordial footprint of the initially pure gas. These new data are combined with the astrophysical models to review the predictability, mass, and chemical composition with regard to stability and existence of the first-generation stars.

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Section: Introductionmentioning

confidence: 89%

Structure and stability of primordial stars

Karafistan¹

2016

Turk J Phys

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“…Paul Ledoux' conjecture was that this instability would lead to finite oscillations, shock waves in the external layers, and mass loss. His result was confirmed and improved by Schwarzschild and Harm in 1959, who repeated Ledoux' computations "on the basis of ... detailed models for massive stars" and did so "not only for homogeneous models appropriate for the initial main sequence but also for inhomogeneous models representing subsequent evolution phases". In the 1970's, numerical studies of the nonlinear effects showed that a star undergoes a swelling and mass losses.…”

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confidence: 84%

An Overview of Paul Ledoux’ Work

Smeyers

2002

International Astronomical Union Colloquium

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“…Above a critical mass, main sequence stars are vibrationally unstable due to the destabilizing effect of nuclear reactions in their central regions (ǫ-mechanism) [11,12]. According to non-linear calculations, such an instability leads to mass loss rather than catastrophic disruption [13][14][15].…”

Section: Vibrational (In-)stability and Mass Lossmentioning

confidence: 99%

“…According to non-linear calculations, such an instability leads to mass loss rather than catastrophic disruption [13][14][15]. Previous investigations of stars of solar-like compositions or slightly metal-poor stars [12,[16][17][18][19][20] indicated that stars above a few 100 M ⊙ would lose a substantial amount of mass during hydrogen burning. However, the structure of metal-free stars Figure 1.…”

Section: Vibrational (In-)stability and Mass Lossmentioning

confidence: 99%

Evolution and nucleosynthesis of very massive primordial stars

Heger¹,

Baraffe²,

Fryer

et al. 2001

Nuclear Physics A

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We investigate the evolution, final fate, and nucleosynthetic yields of rotating and non-rotating very massive stars (VMS) of zero metallicity. First we address the issue of mass loss during hydrogen burning due to vibrational instabilities. We find that these objects are much more stable than what was found in previous studies of VMS of solar composition, and expect only negligible mass loss driven by the pulsations. As these stars thus reach the end of their evolution with massive helium cores, they encounter the pair-creation instability. We find that for helium core masses of ∼ 64 . . . 133 M ⊙ these stars are completely disrupted with explosion energies of up to ∼ 10 53 erg and eject up to ∼ 60 M ⊙ of 56 Ni. Stars with more massive helium cores collapse into black holes. We present the first calculations that follow the collapse of such a massive rotating star and predict that X-ray burst and significant gravitational wave emission could result.

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On the Maximum Mass of Stable Stars.

Cited by 115 publications

References 0 publications

Structure and stability of primordial stars

Structure and stability of primordial stars

An Overview of Paul Ledoux’ Work

Evolution and nucleosynthesis of very massive primordial stars

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