Rubidium-Rich Asymptotic Giant Branch Stars-Reference-Cited by-同舟云学术

Rubidium-Rich Asymptotic Giant Branch Stars

Published:2006-12-15 Issue:5806 Volume:314 Page:1751-1754
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

García-Hernández D. A.¹²³⁴⁵,García-Lario P.¹²³⁴⁵,Plez B.¹²³⁴⁵,D'Antona F.¹²³⁴⁵,Manchado A.¹²³⁴⁵,Trigo-Rodríguez J. M.¹²³⁴⁵

Affiliation:

1. ISO Data Centre, European Space Astronomy Centre, Research and Scientific Support Department, European Space Agency, Villafranca del Castillo, Apdo. 50727, E-28080 Madrid, Spain.

2. Herschel Science Centre, European Space Astronomy Centre, Research and Scientific Support Department, European Space Agency, Villafranca del Castillo, Apdo. 50727, E-28080 Madrid, Spain.

3. Groupe de Recherches en Astronomie et Astrophysique du Languedoc, UMR 5024, Université de Montpellier 2, F-34095 Montpellier Cedex 5, France.

4. INAF–Osservatorio Astronomico di Roma, via Frascati 33, I-00040 MontePorzio Catone, Italy.

5. Instituto de Astrofísica de Canarias and Consejo Superior de Investigaciones Científicas, La Laguna, E-38200 Tenerife, Spain.

Abstract

A long-debated issue concerning the nucleosynthesis of neutron-rich elements in asymptotic giant branch (AGB) stars is the identification of the neutron source. We report intermediate-mass (4 to 8 solar masses) AGB stars in our Galaxy that are rubidium-rich as a result of overproduction of the long-lived radioactive isotope 87 Rb, as predicted theoretically 40 years ago. This finding represents direct observational evidence that the 22 Ne(α,n) 25 Mg reaction must be the dominant neutron source in these stars. These stars challenge our understanding of the late stages of the evolution of intermediate-mass stars and would have promoted a highly variable Rb/Sr environment in the early solar nebula.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

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