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

作者：Huss Gary R^*; Meyer Bradley S; Srinivasan Gopalan; Goswami Jitendra N; Sahijpal Sandeep

来源：Geochimica et Cosmochimica Acta, 2009, 73(17): 4922-4945.

DOI：10.1016/j.gca.2009.01.039

We discuss the possible stellar sources of short-lived radionuclides (SLRs) known to have been present in the early solar system ((26)Al, (36)Cl, (41)Ca, (13)Mn, (60)Fe, (107)Pd, (129)I, (182)Hf, (244)Pu). SLRs produced primarily by irradiation ((7)Be, (10)Be) 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 I to 120 M(circle dot). 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 similar to 20 to similar to 60 M(circle dot) are the most plausible sources. Low-mass AGB stars fail to produce enough (60)Fe. Core-collapse Type 11 supernovae from stars with initial masses of <20 M(circle dot) produce too much (60)Fe and (53)Mn. Sources such as novae, Type la 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 (53)Mn or the r-process elements, so if an AGB star provided the (41)Ca, (36)Cl, (26)Al, (60)Fe, and (107)Pd, and if a late stellar source is required for (53)Mn 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 similar to 110 < A < similar to 130. These can be assigned to SNII explosions of stars of <= 11 M(circle dot) and stars of 12-25 M(circle dot), respectively. More-massive stars, which leave black holes as supernova remnants, apparently do not produce r-process elements.

• 出版日期2009-9-1