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Revista mexicana de física
Print version ISSN 0035-001X
Rev. mex. fis. vol.52 suppl.1 México Jan. 2006
Nucleosynthesis constraints on the First Stars
J. Klappa, D. Bahenac, M.G. CoronaGalindob, H. Dehnend, and S. Galindoa
a Instituto Nacional de Investigaciones Nucleares, Km. 36.5 Carretera MéxicoToluca, 52045 Edo. México, México email: klapp@nuclear.inin.mx, sgu@nuclear.inin.mx
b Instituto Nacional de Astrofísica, Optica y Electronica, Apartado Postal 256, Tonanzintla, Puebla email: mcorona@inaoep.mx
c Charles University Prague, Ke Karlovu 3, 12116 Praha 2, Czech Republic email: bahen@hotmail.com
d Universitat Konstanz, Fachbereich Physik, Fach M568, D78457 Konstanz, Germany email: Heinz.Dehnen@uni-konstanz.de
Recibido el 30 de enero de 2005
Aceptado el 7 de marzo de 2005
Abstract
Star formation and accretion calculations have recently suggested that the first stars are composed of Very Massive Stars (VMS). On the other hand, very massive supernovae (SN) explosion calculations have suggested that the VMS hypothesis is inconsistent with abundance determinations in Extremely Metal Poor (EMP) stars. As an alternative scenario, we propose that the first stars are born very massive but their mass reduced to the Massive Star (MS) range during their hydrogen and helium burning phases. In this paper we present some details of Zero Age Main Sequence (ZAMS) models and evolutionary calculations of a mass losing 5OOM Pop III star. The results indicate that VMS have very high effective temperatures, a large ratio of radiation to total pressure and a luminosity close to the Eddington luminosity and hence, we expect them to have significant radiation driven winds. For conservative evolution our evolutionary tracks are similar to those found in the literature but with the introduction of mass loss the evolution changes strongly and we have shown that VMS can reduce its mass to the MS range if the mass loss parameter N is equal or greater than ~ 300. We have estimated the total amount of matter ejected through winds until the end of the helium burning phase. The proposed scenario suggests that the first stars are born VMS but transformed into MS during their hydrogen and helium burning phases, end as black holes or hypernovae producing the Ferich and rpoor abundances observed in EMP stars, and that could be connected to low redshift gammaray bursts and the reionization of the Universe.
Keywords: Stellar evolution; first stars; population III stars; mass loss.
Resumen
Cálculos recientes de formación estelar y acreción han sugerido que las primeras estrellas están compuestas de Estrellas Muy Masivas (VMS). Por otro lado, cálculos de explosiones de supernovas muy masivas (SN) han sugerido que la hipótesis VMS es inconsistente con determinaciones de abundancias en estrellas Extremadamente Pobres en Metales (EMP). Como un escenario alternativo proponemos que las primeras estrellas nacen como muy masivas, pero su masa es reducida al rango de las estrellas masivas (MS) durante sus fases de quemado de hidrógeno y helio. En este artículo presentamos algunos detalles de modelos de edad cero de la secuencia principal (ZAMS) y cálculos evolutivos de una estrella Pop III de 5OOM con pérdida de masa. Los resultados indican que las VMS tienen temperaturas efectivas muy altas, una alta razón de la presión de radiación a la presión total y una luminosidad cercana a la luminosidad de Eddington y por lo tanto, esperamos que estas estrellas tengan vientos significativos impulsados por radiación. Para evolución conservativa nuestras trayectorias evolutivas son similares a las encontradas en la literatura, pero cuando se introduce pérdida de masa, la evolución cambia fuertemente y hemos demostrado que las VMS pueden reducir su masa al rango de las MS si el parámetro TV de pérdida de masa es igual o mayor que ~ 300. Hemos estimado la cantidad total de materia expulsada a traves de vientos hasta el final de la fase de quemado de helio. El escenario propuesto sugiere que las primeras estrellas nacen como VMS pero son transformadas en MS durante las fases de quemado de hidrógeno y helio, acaban como agujeros negros o hipernovas produciendo las abundancias ricas en Fe y pobres en elementos r que son observadas en estrellas EMP, y que podrían estar relacionadas con ráfagas de rayos gamma con corrimiento al rojo bajo y la reionización del Universo.
Descriptores: Evolución estelar; primeras estrellas; estrellas de población III; pérdida de masa.
PACS: 97.10.Cv; 97.10.Me; 97.10.Xq; 97.20.Wt
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Acknowledgments
We thank Dr. A. Gelover for reading and suggesting improvements to the manuscript. This work has been partially supported by the Mexican Consejo Nacional de Ciencia y Tecnología (CONACyT) under contracts U43534R and J200.476/2004, and the DFG and DAAD of Germany. One of us (D.B.) thank CONACYT for financial support.
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