Standard Solar Composition

Grevesse, N.; Sauval, A. J.

doi:10.1007/978-94-011-4820-7_15

Cited by 173 publications

(227 citation statements)

References 34 publications

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“…We have calculated them for the Grevesse and Sauval (1998) as well as for the Asplund et al (2005) new solar composition. We use standard MLT and FTS convection theory, and employ OPAL and Irwin-EOS.…”

Section: The Garsom Standard Solar Modelmentioning

confidence: 99%

GARSTEC—the Garching Stellar Evolution Code

Weiß

Schlattl

2007

Astrophys Space Sci

289

271

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Section: The Garsom Standard Solar Modelmentioning

confidence: 99%

GARSTEC—the Garching Stellar Evolution Code

Weiß

Schlattl

2007

Astrophys Space Sci

289

271

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“…Using the standard photospheric solar abundances 16 we obtain the metallicity of these elements as [ (cm 22 )] < 21.3 is assumed from a damped Lya system model for the Lya damping wing presented below. These values may not represent the typical abundances in the GRB host galaxy for several reasons.…”

mentioning

confidence: 99%

An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295

Kawai

Kosugi

Aoki

et al. 2006

Nature

256

191

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“…The more recent Solar abundance determinations of O, Ne, and Fe by Lodders (2003) are ∼30% lower than those given by Anders and Grevesse (1989). The Solar abundances of O and Ne reported by Grevesse and Sauval (1998) are higher and the abundance of Fe is slightly lower than those reported by Lodders (2003).…”

Section: What Chemical Abundance Measurements Tell Usmentioning

confidence: 64%

“…Dupke and White (2000) and Dupke and Arnaud (2001) used the Ni/Fe ratio measured in clusters by ASCA to distinguish between the SN Ia models assuming slow deflagration and delayed detonation. While the deflagration explosion mechanism of SN Ia (represented by the W7 and W70 models in the literature, Iwamoto et al 1999) predicts high Ni/Fe ratio of 2.18-3.22 in the Solar units of Grevesse and Sauval (1998), the delayed-detonation explosion scenarios predict significantly lower Ni/Fe ratios of 0.9-1.4 Solar. They are represented by the WDD1, WDD2, WDD3, CDD1, and CDD2 models in the literature, where the last digit indicates the density at which the flame velocity becomes supersonic (deflagration-to-detonation transition density) in units of 10 7 g cm −3 ; the "C" and "W" refer to two different central densities (1.37 × 10 9 and 2.12 × 10 9 g cm −3 , respectively) in the model at the onset of the thermonuclear runaway (Iwamoto et al 1999).…”

Section: Constraining Supernova Models Using Clustersmentioning

confidence: 99%

X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories

Böhringer

Werner

2009

Astron Astrophys Rev

195

142

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Galaxy clusters, the largest clearly defined objects in our Universe, are ideal laboratories to study in detail the cosmic evolution of the intergalactic intracluster medium (ICM) and the cluster galaxy population. For the ICM, which is heated to X-ray radiating temperatures, X-ray spectroscopy is the most important tool to obtain insight into the structure and astrophysics of galaxy clusters. The ICM is also the hottest plasma that can be well studied under thermal equilibrium conditions. In this review we recall the basic principles of the interpretation of X-ray spectra from a hot, tenuous plasma and we illustrate the wide range of scientific applications of X-ray spectroscopy. The determination of galaxy cluster masses, the most important prerequisite for using clusters in cosmological studies, rest crucially on a precise spectroscopic determination of the ICM temperature distribution. The study of the thermal structure of the ICM provides a very interesting fossil record of the energy release during galaxy formation and evolution, giving important constraints on galaxy formation models. The temperature and pressure distribution of the ICM gives us important insight into the process of galaxy cluster merging and the dissipation of the merger energy in form of turbulent motion. Cooling cores in the centers of about half of the cluster population are interesting laboratories to investigate the interplay between gas cooling, star-and black hole formation and energy feedback, which is diagnosed by means of X-ray spectroscopy. The element abundances deduced from X-ray spectra of the ICM provide a cosmic history record of the contribution of different supernovae to the nucleosynthesis of heavy elements and their spatial distribution partly reflects important transport processes in the ICM. Some discussion of plasma diagnostics for conditions out of thermal equilibrium and an outlook on the future prospects of X-ray spectroscopic cluster studies complete our review.

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Standard Solar Composition

Cited by 173 publications

References 34 publications

GARSTEC—the Garching Stellar Evolution Code

GARSTEC—the Garching Stellar Evolution Code

An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295

X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories

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