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What do we do when models don't fit? On model atmospheres and real stellar spectra
Uppsala University, Teknisk-naturvetenskapliga vetenskapsområdet, Faculty of Science and Technology, Astronomical observatory.
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1997 (English)In: FUNDAMENTAL STELLAR PROPERTIES: THE INTERACTION BETWEEN OBSERVATION AND THEORY, ISSN 0074-1809, no 189, 261-276 p.Article in journal (Other scientific) Published
Abstract [en]

Developments in the modelling of stellar atmospheres and results from the confrontation between calculated and observed fluxes and spectra are discussed. It is argued that, although impressive advances in the study of O-type, WR and cool star spectra have

Place, publisher, year, edition, pages
KLUWER ACADEMIC PUBL , 1997. no 189, 261-276 p.
Keyword [en]
COOL DWARF STARS; INCLUDING SPHERICAL EXTENSION; RADIATION-DRIVEN WINDS; BALMER-LINE-PROFILES; IRON-GROUP ELEMENTS; HOT LUMINOUS STARS; SOLAR GRANULATION; CARBON STARS; O-STARS; VEGA
Identifiers
URN: urn:nbn:se:uu:diva-85334OAI: oai:DiVA.org:uu-85334DiVA: diva2:113242
Note
Addresses: Gustafsson B, UNIV UPPSALA, ASTRON OBSERV, BOX 515, S-75120 UPPSALA, SWEDEN. OBSERV PARIS, MEUDON, FRANCE. UNIV MARYLAND, COLLEGE PK, MD 20742. INST THEORET ASTROPHYS, D-6900 HEIDELBERG, GERMANY.Available from: 2008-10-17 Created: 2008-10-17 Last updated: 2011-01-15

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