主要内容:
如果是大原子量的原子放射性衰变作为GRB 130603B的余辉辐射的话，那么原子量大于130的那些放射性元素可能主要就是这个过程产生的。
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文章信息:
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- · arXiv e-print (arXiv:1401.2166)
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| Title: |
| Implications of GRB 130603B and its macronova for r-process nucleosynthesis |
| Authors: |
| Piran, Tsvi; Korobkin, Oleg; Rosswog, Stephan |
| Publication: |
| eprint arXiv:1401.2166 |
| Publication Date: |
| 01/2014 |
| Origin: |
| ARXIV |
| Keywords: |
| Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology, Nuclear Theory |
| Bibliographic Code: |
| 2014arXiv1401.2166P |
Abstract
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.
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