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We have computed the evolution of Super-AGB stars from the main sequenceand up to a few hundred thermal pulses, with special attention to the low metallicity cases(Z = 10 10; 10 5; 10 4 and 10 3). Our computations have been performed using time–dependent mixing and new opacity tables that admit variations in the abundances of carbonand oxygen. By following the evolution along the main central burning stages and theearly TP-SAGB, we resolve the upper mass limits for the formation of TP-SAGB stars anddetermine the mass range at which the dredge-out phenomenon occurs. This phenomenoninvolves the merger of a convective shell sustained by helium burning at the top of thedegenerate core with the hydrogen–rich convective envelope and the occurrence of a hydrogenflash. The dredge–out allows elements synthesised through helium burning to betransported to the stellar surfaces and therefore it can a ect the initial composition of theTP-SAGB stars.

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Autor(es)

Gil Pons, Pilar -  Doherty, Carolyn L. - 

Id.: 55271627

Idioma: inglés  - 

Versión: 1.0

Estado: Final

Palabras claveÀrees temàtiques de la UPC -  Física -  Astronomia i astrofísica - 

Tipo de recurso: Article  - 

Tipo de Interactividad: Expositivo

Nivel de Interactividad: muy bajo

Audiencia: Estudiante  -  Profesor  -  Autor  - 

Estructura: Atomic

Coste: no

Copyright: sí

: Open Access

Requerimientos técnicos:  Browser: Any - 

Fecha de contribución: 06-may-2012

Contacto:

Localización:

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  2. Super and massive AGB stars - III. nucleosynthesis in metal-poor and very metal-poor stars - Z = 0.001 and 0.0001 We present a new grid of stellar models and nucleosynthetic yields for super-AGB stars with metallic...
  3. Evolution and CNO yields of Z = 10-5 stars and possible effects on carbon-enhanced metal-poor production Aims. Our main goals are to get a deeper insight into the evolution and final fates of intermediate-...
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  5. The evolution and C, N and O yields of intermediate-mass Z = 10-5 stars in isolation and in close binary systems We have computed the evolution of Z = 10−5 stars of masses between 4 and 9 M , from their main seque...

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