Stellar Structure and Evolution

Kippenhahn, Rudolf; Weigert, Alfred; Weiß, Achim

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

Cited by 901 publications

(839 citation statements)

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“…5). Although the influence of initial helium abundance on the stellar properties has already been extensively described in the literature (e.g., Iben & Faulkner 1968;Iben & Rood 1969;Demarque et al 1971;Sweigart 1978;D'Antona et al 2005;Caloi & D'Antona 2007;Salaris & Cassisi 2005;Maeder 2009;Pietrinferni et al 2009;Sbordone et al 2011;Valcarce et al 2012;Cassisi et al 2013;Kippenhahn et al 2013), to our knowledge this is the first investigation of the impact of helium content higher than ∼0.42 on the whole evolution (from the pre-main sequence to the end of the AGB phase) at low [Fe/H], and for such a broad mass range 4 .…”

Section: Objectives Of the Present Series Of Papersmentioning

confidence: 93%

Evolution of long-lived globular cluster stars

Chantereau

Charbonnel

Decressin

2015

A&A

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Context. Our understanding of the formation and early evolution of globular clusters (GCs) has been totally overthrown with the discovery of the peculiar chemical properties of their long-lived host stars. Aims. As a consequence, the interpretation of the observed color-magnitude diagrams and of the properties of the GC stellar populations requires the use of stellar models computed with relevant chemical compositions.Methods. We present a grid of 224 stellar evolution models for low-mass stars with initial masses between 0.3 and 1.0 M and initial helium mass fraction between 0.248 and 0.8 computed for [Fe/H] = -1.75 with the stellar evolution code STAREVOL. This grid is made available to the community. Results. We explore the implications of the assumed initial chemical distribution for the main properties of the stellar models: evolution paths in the Hertzsprung-Russel diagram (HRD), duration and characteristics of the main evolutionary phases, and the chemical nature of the white dwarf remnants. We also provide the ranges in initial stellar mass and helium content of the stars that populate the different regions of the HRD at the ages of 10 and 13.4 Gyr, which are typical for Galactic GCs.

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Section: Objectives Of the Present Series Of Papersmentioning

confidence: 93%

Evolution of long-lived globular cluster stars

Chantereau

Charbonnel

Decressin

2015

A&A

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“…The equilibrium is guaranteed by the balance between the pressure gradient and the force of gravity -the pressure being provided by a combination of radiation, ideal gas and partially or totally degenerate electrons. Since the star loses energy, because it is hotter than the environment and/or because of the neutrino losses, it heats up and shrinks at the same time, according to the virial theorem, i.e., a fraction of the gravitational energy gained by the contraction goes into internal energy while the remaining fraction replaces the energy lost [8]. When the central temperature is high enough, thermonuclear fusion reactions take place, nuclear energy supplies the energy lost, and gravitational contraction halts.…”

Section: Massive Stars: Distinctive Featuresmentioning

confidence: 99%

Supernovae from Massive Stars

Limongi¹

2017

Handbook of Supernovae

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Massive stars, by which we mean those stars exploding as core collapse supernovae, play a pivotal role in the evolution of the Universe. Therefore, the understanding of their evolution and explosion is fundamental in many branches of physics and astrophysics, among which, galaxy evolution, nucleosynthesis, supernovae, neutron stars and pulsars, black holes, neutrinos and gravitational waves. In this chapter, the author presents an overview of the presupernova evolution of stars in the range between 13 and 120 M ⊙ , with initial metallicities between [Fe/H]=-3 and [Fe/H]=0 and initial rotation velocities v = 0, 150, 300 km/s. Emphasis is placed upon those evolutionary properties that determine the final fate of the star with special attention to the interplay among mass loss, mixing and rotation. A general picture of the evolution and outcome of a generation of massive stars, as a function of the initial mass, metallicity and rotation velocity, is finally outlined.

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“…Fig. 22.7 in Kippenhahn et al 2012). We first confronted the parameters of LL Aqr with the PAdova and TRieste Stellar Evolution Code (PARSEC) isochrones (Bressan et al 2012), then with stellar evolutionary tracks computed with the Modules for Experiments in Stellar Astrophysics (MESA) (e.g.…”

Section: Stellar Evolution Models For Ll Aqrmentioning

confidence: 99%

A solar twin in the eclipsing binary LL Aquarii

Graczyk

Smolec

Pavlovski

et al. 2016

A&A

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Aims. In the course of a project to study eclipsing binary stars in vinicity of the Sun, we found that the cooler component of LL Aqr is a solar twin candidate. This is the first known star with properties of a solar twin existing in a non-interacting eclipsing binary, offering an excellent opportunity to fully characterise its physical properties with very high precision. Methods. We used extensive multi-band, archival photometry and the Super-WASP project and high-resolution spectroscopy obtained from the HARPS and CORALIE spectrographs. The spectra of both components were decomposed and a detailed LTE abundance analysis was performed. The light and radial velocity curves were simultanously analysed with the Wilson-Devinney code. The resulting highly precise stellar parameters were used for a detailed comparison with PARSEC, MESA, and garstec stellar evolution models.Results. LL Aqr consists of two main-sequence stars (F9 V + G3 V) with masses of M 1 = 1.1949 ± 0.0007 and M 2 = 1.0337 ± 0.0007 M , radii R 1 = 1.321±0.006 and R 2 = 1.002±0.005 R , temperatures T 1 = 6080±45 and T 2 = 5703±50 K and solar chemical composition [M/H] = 0.02 ± 0.05. The absolute dimensions, radiative and photometric properties, and atmospheric abundances of the secondary are all fully consistent with being a solar twin. Both stars are cooler by about 3.5σ or less metal abundant by 5σ than predicted by standard sets of stellar evolution models. When advanced modelling was performed, we found that full agreement with observations can only be obtained for values of the mixing length and envelope overshooting parameters that are hard to accept. The most reasonable and physically justified model fits found with MESA and garstec codes still have discrepancies with observations but only at the level of 1σ. The system is significantly younger that the Sun, with an age between 2.3 Gyr and 2.7 Gyr, which agrees well with the relatively high lithium abundance of the secondary, A(Li) = 1.65 ± 0.10 dex.

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Stellar Structure and Evolution

Cited by 901 publications

References 0 publications

Evolution of long-lived globular cluster stars

Evolution of long-lived globular cluster stars

Supernovae from Massive Stars

A solar twin in the eclipsing binary LL Aquarii

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