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Injection of freshly synthesized Ca-41 in the early solar nebula by an asymptotic giant branch star
Wasserburg, G. J.; Gallino, R.; Busso, M.; Goswami, J. N.; Raiteri, C. M.
AA(California Inst. of Technology, Pasadena, CA, US), AB(California Inst. of Technology, Pasadena, CA, US), AC(Osservatorio Astronomico di Torino, Torino, Italy), AD(Osservatorio Astronomico di Torino, Torino, Italy), AE(Osservatorio Astronomico di Torino, Torino, Italy)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 440, no. 2, p. L101-L104 (ApJL Homepage)
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NASA/STI Keywords:
Abundance, Asymptotic Giant Branch Stars, Calcium Isotopes, Molecular Clouds, Solar System Evolution, Aluminum 26, Nuclear Fusion
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We show that ejecta from the envelope of one asymptotic giant branch star of M is approximately 3 solar mass may account for many of the short-lived nuclei in the early solar system and also for the recent evidence of the presence of Ca-41 (bar-tau41 = 1.50 x 105 yr) in early solar nebular condensates. This would require that the injection into the protosolar molecular cloud took place within a narrow time interval of (5-7) x 105 yr before the formation of the solar system. If true, this places extremely tight constraints on the whole process of injection mixing and collapse. The timescales for both Ca-41 and Al-26 require that the placental medium be a dense molecular cloud (2 x 103 -8 x 103( H/cc. If the observed residual Ca-41 is instead produced by a proton bombardment mechanism within the early solar system, similar to what appears necessary to explain Mn-53, then the time interval is relaxed but would still be (1-2) x 106 yr from consideration of Al-26.

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