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The Evolution of 3He, 4He and D in the Galaxy

Published online by Cambridge University Press:  25 May 2016

Cristina Chiappini  and
Francesca Matteucci
Cristina Chiappini
Affiliation:
Depto. Astronomia - Observatório National, R. Gal. José Cristino 77 - CEP 20921-400 - Rio de Janeiro - RJ - Brazil
Francesca Matteucci
Affiliation:
Dipartimento di Astronomia, Università di Trieste, Via G. B. Tiepolo 11 - 34100 Trieste, Italy

Abstract

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In this work we present the predictions of a modified version of the ‘two-infall model’ (Chiappini et al. 1997 - CMG) for the evolution of 3He, 4He and D in the solar vicinity, as well as their distributions along the Galactic disk. In particular, we show that when allowing for extra-mixing process in low mass stars (M < 2.5 M⊙), as predicted by Charbonnel and do Nascimento (1998), a long standing problem in chemical evolution is solved, namely: the overproduction of 3He by the chemical evolution models as compared to the observed values in the sun and in the interstellar medium. Moreover, we show that chemical evolution models can constrain the primordial value of the deuterium abundance and that a value of (D/H)p < 3 × 10—5 is suggested by the present model. Finally, adopting the primordial 4He abundance suggested by Viegas et al. (1999), we obtain a value for ΔY/ΔZ ≃ 2 and a better agreement with the solar 4He abundance.

Type
7. Evolution of the Light Elements
Information
Symposium - International Astronomical Union , Volume 198: The Light Elements and their Evolution , 2000 , pp. 540 - 546
Copyright
Copyright © Astronomical Society of the Pacific 2000 

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