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Single and binary evolution of Population III stars and their supernova explosions

Author
LAWLOR, T. M1 ; YOUNG, T. R2 ; JOHNSON, T. A3 ; MACDONALD, J4
[1] Department of Physics, Penn State University, Brandywine, Media, PA 19063, United States
[2] Department of Physics, University of North Dakota, Grand Forks, ND 58202, United States
[3] Department of Math, Science & Technology, University of Minnesota, Crookston, Crookston, MN 56716, United States
[4] Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, United States
Source

Monthly Notices of the Royal Astronomical Society. 2008, Vol 384, Num 4, pp 1533-1543, 11 p ; ref : 1/2 p

CODEN
MNRAA4
ISSN
0035-8711
Scientific domain
Astronomy earth cosmic environment
Publisher
Blackwell Science, Oxford
Publication country
United Kingdom
Document type
Article
Language
English
Author keyword
binaries: general stars: evolution supernovae: general
Keyword (fr)
Abondance solaire Abondance stellaire Abondance élément Accrétion Binaire Courbe lumière Elément lourd Etoile M Evolution stellaire Explosion supernova Modèle stellaire Population type III Supernova
Keyword (en)
Solar abundance Stellar abundance Element abundance Accretion Binary stars Light curves Heavy element M stars Stellar evolution Supernovae explosion Star models Population III Supernovae
Keyword (es)
Abundancia solar Abundancia estelar Elemento pesado Explosión supernova Población estelar III
Classification
Pascal
001 Exact sciences and technology / 001E Earth, ocean, space / 001E03 Astronomy

Discipline
Astronomy
Origin
Inist-CNRS
Database
PASCAL
INIST identifier
20181395

Sauf mention contraire ci-dessus, le contenu de cette notice bibliographique peut être utilisé dans le cadre d’une licence CC BY 4.0 Inist-CNRS / Unless otherwise stated above, the content of this bibliographic record may be used under a CC BY 4.0 licence by Inist-CNRS / A menos que se haya señalado antes, el contenido de este registro bibliográfico puede ser utilizado al amparo de una licencia CC BY 4.0 Inist-CNRS

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