The Abundances of the Elements in the Solar Atmosphere.

Goldberg, Leo; Müller, Edith A.; Aller, L. H.

doi:10.1086/190053

Cited by 256 publications

(54 citation statements)

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“…It thus seems that th+ particles which reach the earth's orbit mainly consist of protons. The P/a ratio for F-type events sometimes attains values of 50 or more and so seems to be different from and greater than the chemical abundance in the photosphere and the corona of the sun which has been estimated to be 6 or 7 by spectroscopic methods (e.g., Aller, 1961Aller, , 1965Goldberg, Muller and It 11 Aller, 1963, Muller, 1966Pottasch, 1964Pottasch, , 1966Unsold, 1969).…”

Section: Observational Results and Their I Rplicav Ionmentioning

confidence: 90%

The acceleration and propagation of solar cosmic rays as deduced from the relative abundance of protons to helium nuclei

Sakurai

1971

Sol Phys

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Except for protons, the chemical composition of solar cosmic rays is very similar to the abundance of the elements at the photosphere of the sun. If we consider the relative abundance ratio of protons to a-particles (P/a) at constant rigidity, this ratio is highly variable from one solar cosmic ray event to another. This ratio observed at the earth, The chemical composition and rigidity spectra of solar cosmic rays suggest that solar cosmic rays are mainly accelerated by the Fermi mechanism in solar flares. The jbserved variation of P/a's is produced mainly through the difference between the propagation characteristics of protons and a-particles.

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Section: Observational Results and Their I Rplicav Ionmentioning

confidence: 90%

The acceleration and propagation of solar cosmic rays as deduced from the relative abundance of protons to helium nuclei

Sakurai

1971

Sol Phys

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“…Several analyses of the solar Zr abundance, made before 1980, used Corliss & Bozman (1962) log gf (Aller 1965;Wallerstein 1966;Grevesse et al 1968) or older ones (Goldberg et al 1960) or have been made to derive a temperature correction for the Corliss & Bozman (1962) data (Allen 1976). The use of these transition probabilities, which are known to contain errors depending on excitation and temperature, coupled with the use of old solar spectral atlases, explains discrepancies of these Zr abundance determinations based either on Zr I and/or Zr II.…”

Section: Solar Zr Abundance In the Literaturementioning

confidence: 99%

The solar photospheric abundance of zirconium

et al. 2011

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Zirconium (Zr), together with strontium and yttrium, is an important element in the understanding of the Galactic nucleosynthesis. In fact, the triad Sr-Y-Zr constitutes the first peak of s-process elements. Despite its general relevance not many studies of the solar abundance of Zr were conducted. We derive the zirconium abundance in the solar photosphere with the same CO 5 BOLD hydrodynamical model of the solar atmosphere that we previously used to investigate the abundances of C-N-O. We review the zirconium lines available in the observed solar spectra and select a sample of lines to determine the zirconium abundance, considering lines of neutral and singly ionised zirconium. We apply different line profile fitting strategies for a reliable analysis of Zr lines that are blended by lines of other elements. The abundance obtained from lines of neutral zirconium is very uncertain because these lines are commonly blended and weak in the solar spectrum. However, we believe that some lines of ionised zirconium are reliable abundance indicators. Restricting the set to Zr II lines, from the CO 5 BOLD 3D model atmosphere we derive A(Zr) = 2.62 ± 0.06, where the quoted error is the RMS line-to-line scatter.

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“…The classic compilation of abundances determined from photospheric absorption lines is the work of Goldberg, Muller, and Aller (1960). No Garwood and Evans (1974), and the Ge abundance that of Ross and Aller (1974 (1974a.…”

Section: The Boron Value Inmentioning

confidence: 99%