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    Alley-side Pickup: 10am - 7pm

    3038 Hennepin Ave Minneapolis, MN
    612-822-4611

Open Daily: 10am - 10pm | Alley-side Pickup: 10am - 7pm
3038 Hennepin Ave Minneapolis, MN
612-822-4611
Solar Composition and Its Evolution -- From Core to Corona: Proceedings of an Issi Workshop 26-30 January 1998, Bern, Switzerland

Solar Composition and Its Evolution -- From Core to Corona: Proceedings of an Issi Workshop 26-30 January 1998, Bern, Switzerland

Solanki, S. K.
Huber, M.
Fröhlich, Claus

Hardcover

Series: Space Sciences Issi, Book 5

Astronomy & SpacePhysics

ISBN10: 0792354966
ISBN13: 9780792354963
Publisher: Springer Nature
Published: Dec 31 1998
Pages: 431
Weight: 1.76
Height: 1.00 Width: 6.14 Depth: 9.21
Language: English
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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