Abundances of the Elements in the Sun

Grevesse, N.; Sauval, A. J.

doi:10.1007/0-306-46927-8_23

Cited by 36 publications

(50 citation statements)

References 57 publications

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“…The NLTE profiles of the Mg I lines computed with log(Mg/H) = 7.57 agree well with the solar spectrum (see Fig. 1) in good agreement with the determinations of Grevesse & Sauval (2000), and of Shimanskaya (2000) who found log(Mg/H) = 7.58. The potassium lines are also well reproduced by our calculations (see Fig.…”

Section: Fit Of the Solar Spectrumsupporting

confidence: 85%

“…An "m" in the last column of the table means that the atmosphere of the star (giant) has been found "mixed" with the deep hydrogen burning layer by Spite et al (2005Spite et al ( , 2006a. For the determination of the relative LTE and NLTE abundances, we adopted in this table the solar values log(Mg/H) = 7.58 and log(K/H) = 5.12 following Grevesse & Sauval (2000) for a better homogeneity with the previous LTE determinations ).…”

Section: Atmospheric Parametersmentioning

confidence: 99%

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Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way

Andrievsky¹,

Spite²,

Коротин³

et al. 2010

A&A

123

126

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Aims. LTE abundances of light elements in extremely metal-poor (EMP) stars have been previously derived from high quality spectra. New derivations, free from the NLTE effects, will better constrain the models of the Galactic chemical evolution and the yields of the very first supernovae. Methods. The NLTE profiles of the magnesium and potassium lines have been computed in a sample of 53 extremely metal-poor stars with a modified version of the program MULTI and adjusted to the observed lines in order to derive the abundances of these elements. Results. The NLTE corrections for magnesium and potassium are in good agreement with the works found in the literature. The abundances are slightly changed, reaching a better precision: the scatter around the mean of the abundance ratios has decreased. Magnesium may be used with confidence as reference element. Together with previously determined NLTE abundances of sodium and aluminum, the new ratios are displayed, for comparison, along the theoretical trends proposed by some models of the chemical evolution of the Galaxy, using different models of supernovae.

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Section: Fit Of the Solar Spectrumsupporting

confidence: 85%

Section: Atmospheric Parametersmentioning

confidence: 99%

Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way

Andrievsky¹,

Spite²,

Коротин³

et al. 2010

A&A

123

126

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“…The first is that the element abundance in the accretion flow is the same as that in the solar atmosphere (Grevesse & Sauval 2000). The companion of the stellar mass black hole could be a main-sequence star, and the accretion matter of a supermassive black hole at the galactic center is presumably supplied by a number of nearby stars.…”

Section: Calculation Of Nuclear Reaction Heatingmentioning

confidence: 99%

Is the energy generation rate of nuclear reactions in hot accretion flows important?

Zhang¹,

Wang²,

Yuan³

et al. 2009

A&A

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The temperature of hot accretion flows around black holes is sufficiently high for the ignition of nuclear reactions. This is potentially an important nucleosynthesis mechanism in the universe. As the first step in studying this problem, we need to measure physical quantities such as density and temperature of the accretion flow. In usual studies of the hot accretion flow, viscous dissipation is considered to be the only heating mechanism, while the heating caused by nuclear reactions is not considered. In this paper, we investigate whether the energy generation rate of nuclear reaction is important compared to the viscous heating. Our calculation indicates that the former is at most one percent of the latter and thus is not important. The dynamics of accretion flow can be therefore calculated in the usual way, without the need to consider heating due to nuclear reactions.

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“…Input physics: The  equation of state (Eggleton et al 1973) was used, together with opacities determined by Rogers et al (1996) using the solar mixture of Grevesse & Noels (1993), complemented at low temperatures by Alexander & Ferguson (1994) opacities. In the convection zones the mixing is insured by a large turbulent diffusion coefficient and the temperature gradient is computed according to the Böhm-Vitense (1958) convection theory; the mixing-length parameter is fixed to the value in the standard solar model computed with the same physics 3 .…”

Section: Computation Of Models and Physical Inputsmentioning

confidence: 99%

“…The first simulates the metals heavier than potassium. For the solar mixture of Grevesse & Noels (1993) used so far, their mean 4 charge and mean atomic weight are respectively 26 and 55. Therefore, a dummy "iron", labeled hereafter { 55 Fe}, is well representative of the heaviest chemical species.…”

Section: Computation Of Models and Physical Inputsmentioning

confidence: 99%

Atomic diffusion in star models of type earlier than G

Morel

Thévenin

2002

A&A

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Abstract. We introduce the mixing resulting from the radiative diffusivity associated with the radiative viscosity in the calculation of stellar evolution models. We find that the radiative diffusivity significantly diminishes the efficiency of the gravitational settling in the external layers of stellar models corresponding to types earlier than ≈G. The surface abundances of chemical species predicted by the models are successfully compared with the abundances determined in members of the Hyades open cluster. Our modeling depends on an efficiency parameter, which is evaluated to a value close to unity, that we calibrate in this study.

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Abundances of the Elements in the Sun

Cited by 36 publications

References 57 publications

Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way

Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way

Is the energy generation rate of nuclear reactions in hot accretion flows important?

Atomic diffusion in star models of type earlier than G

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