http://arxiv.org/abs/1401.2166
The tentative identification of a Li-Paczynski macronova following the short GRB 130603B indicated that a few hundredths of a solar mass of neutron star matter were ejected and that this ejected mass has radioactively decayed into heavy r-process elements. If correct, this confirms long standing predictions (Eichler, Livio, Piran and Schramm 1989) that on the one hand, sGRBs are produced in compact binary mergers (CBMs) and on the other hand that these events are significant and possibly dominant sources of the heavy (A>130) r-process nuclei. Assuming that this interpretation is correct we obtain a lower limit of 0.02 m_sun on the ejected mass. Using the current estimates of the rate of sGRBs and with a beaming factor of 50, mergers associated with sGRBs can produce all the observed heavy r-process material in the Universe. We confront this conclusion with cosmochemistry and show that even though such events are rare, mixing is sufficient to account for the current homogeneous distribution of r-process material in the Galaxy. However, the appearance of significant amounts of Eu in some very low metallicity stars requires that some mergers took place very early on, namely with a very short time delay after the earliest star formation episodes. Alternatively, an additional early r-processsource may have contributed at that early stage. Finally, we note that evidence for short lived {244}^Pu in the very early solar system suggests that a merger of this kind took place within the vicinity of the solar system shortly (a few hundred million years) before its formation.
Mon, 13 Jan 14
25/39
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