Stellar sources of the short-lived radionuclides in the early solar system

Huss, Gary R. ; Meyer, Bradley S. ; Srinivasan, Gopalan ; Goswami, Jitendra N. ; Sahijpal, Sandeep (2009) Stellar sources of the short-lived radionuclides in the early solar system Geochimica et Cosmochimica Acta, 73 (17). pp. 4922-4945. ISSN 0016-7037

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We discuss the possible stellar sources of short-lived radionuclides (SLRs) known to have been present in the early solar system (26Al, 36Cl, 41Ca, 53Mn, 60Fe, 107Pd, 129I, 182Hf, 244Pu). SLRs produced primarily by irradiation (7Be, 10Be) are not discussed in this paper. We evaluate the role of the galactic background in explaining the inventory of SLRs in the early solar system. We review the nucleosynthetic processes that produce the different SLRs and place the processes in the context of stellar evolution of stars from 1 to 120 M. The ejection of newly synthesized SLRs from these stars is also discussed. We then examine the extent to which each stellar source can, by itself, explain the relative abundances of the different SLRs in the early solar system, and the probability that each source would have been in the right place at the right time to provide the SLRs. We conclude that intermediate-mass AGB stars and massive stars in the range from ~20 to ~60 M are the most plausible sources. Low-mass AGB stars fail to produce enough 60Fe. Core-collapse Type II supernovae from stars with initial masses of 20 M produce too much 60Fe and 53Mn. Sources such as novae, Type Ia supernovae, and core-collapse supernovae of O-Ne-Mg white dwarfs do not appear to provide the SLRs in the correct proportions. However, intermediate-mass AGB stars cannot provide 53Mn or the r-process elements, so if an AGB star provided the 41Ca, 36Cl, 26Al, 60Fe, and 107Pd, and if a late stellar source is required for 53Mn and the r-process elements, then two types of sources would be required. A separate discussion of the production of r-process elements highlights the difficulties in modeling their production. There appear to be two sources of r-process elements, one that produces the heavy r-process elements, including the actinides, and one that produces the elements from N to Ge and the elements ~110 A ~130. These can be assigned to SNII explosions of stars of ≤11 M and stars of 12-25 M, respectively. More-massive stars, which leave black holes as supernova remnants, apparently do not produce r-process elements.

Item Type:Article
Source:Copyright of this article belongs to Geological Society of America.
ID Code:14646
Deposited On:12 Nov 2010 13:54
Last Modified:02 Jun 2011 08:20

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