the chemical history of the elements iisya28/lecciones/manuel_1.pdf · • iii.big-bang...
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THE CHEMICAL HISTORY OF THE ELEMENTS I
Manuel PeimbertInstituto de Astronomía, UNAM
El Colegio Nacional
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OVERVIEW• I Introduction• II. Observational constraints based on H II
Regions and Planetary Nebulae• III.Big-Bang Nucleosynthesis and the Primordial
Helium Abundance• IV.Pagel´s method to derive the O/H ratio in
galaxies• V.Chemical Evolution of the Galaxy: C,O, and N
Gradients
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Bibliography
• Nucleosynthesis and Chemical Evolution ofGalaxies. B.E.J. Pagel, 1997
• Astrophysics of Gaseous Nebulae and Active Galactic Nuclei. D. E. Osterbrock, 1989
• Astrophysics of Gaseous Nebulae and Active Galactic Nuclei III. D. E. Osterbrock and G. Ferland, 2005
• http://nedwww.ipac.caltech.edu/level5/
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pi
Hirschi, Meynet & Maeder (2005)
Yields. Estrellas aisladas. MS
10 < m < 20 rotación mas importante que vientosm > 30 viento mas importante que rotación
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Importancia de la IMF
Yields. Estrellas aisladas. MS
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Yields. Estrellas aisladas. Pop III
Pop III (Z ~ 0)
• Woosley & Weaver (1995)
• Abia et al. (2001)
• Meynet & Maeder (2002)
• Heger & Woosley (2002)
• Marigo et al. (2003)
• Umeda & Nomoto (2003)
• Chieffi & Limongi (2004)
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M bariónica y M no bariónica
Evolución química considera sólo M bariónica
•Acreción debido a Potencial Gravitacional
•Viento debido a que la E térmica del ISM ≥ E gravitacional
Materia no bariónica
Materia bariónica
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