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Solar Composition and its Evolution - from Core to Corona - Proceedings of an ISSI Workshop 26-30 January 1998, Bern, Switzerland (Hardcover, Reprinted from SPACE SCIENCE REVIEWS, 85:1-2, 1999)
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Solar Composition and its Evolution - from Core to Corona - Proceedings of an ISSI Workshop 26-30 January 1998, Bern, Switzerland (Hardcover, Reprinted from SPACE SCIENCE REVIEWS, 85:1-2, 1999)
Series: Space Sciences Series of ISSI, 5
Expected to ship within 10 - 15 working days
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The discovery of chemical elements in celestial bodies and the
first estimates of the chemical composition of the solar atmosphere
were early results of Astrophysics - the subdiscipline of Astronomy
that was originally concerned with the general laws of radiation
and with spectroscopy. Following the initial quantitative abundance
studies by Henry Norris Russell and by Cecilia Payne-Gaposchkin, a
tremendous amount of theoretical, observa tional, laboratory and
computational work led to a steadily improving body of knowledge of
photospheric abundances - a body of knowledge that served to guide
the theory of stellar evolution. Solar abundances determined from
photospheric spectra, together with the very similar abundances
determined from carbonaceous chondrites (where extensive
information on isotopic composition is available as well), are
nowadays the reference for all cosmic composition measures. Early
astrophysical studies of the solar photospheric composition made
use of atmosphere models and atomic data. Consistent abundances
derived from different atmospheric layers and from lines of
different strength helped to confirm and estab lish both models and
atomic data, and eventually led to the now accepted, so-called
"absolute" abundance values - which, for practical reasons,
however, are usually given relative to the number of hydrogen
nuclei.
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