Volume 471, Number 1, August III 2007
|Page(s)||227 - 236|
|Section||Stellar structure and evolution|
|Published online||06 June 2007|
Nucleosynthesis in neutron-rich ejecta from quark-novae
Department of Physics and Astronomy, Ohio University, Athens, OH 45701, USA e-mail: firstname.lastname@example.org
2 Department of Physics and Astronomy, Clemson University, Clemson, SC 29634, USA
3 Department of Astronomy and Astrophysics, Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
4 Department of Physics and Astronomy, University of Calgary, 2500 University Drive NW, Calgary, Alberta, T2N 1N4, Canada
Accepted: 23 May 2007
We explore heavy-element nucleosynthesis by rapid neutron capture (r-process) in the decompressing ejecta from the surface of a neutron star. The decompression is triggered by a violent phase transition to strange quark matter (quark-nova scenario). The presence of neutron-rich large Z nuclei (40,95) < < (70,177), the large neutron-to-seed ratio, and the low electron fraction Ye ~ 0.03 in the decompressing ejecta present favorable conditions for the r-process. We perform network calculations that are adapted to the quark-nova conditions, and which mimic usual equilibrium r-process calculations during the initially cold decompression phase. They match to dynamical r-process calculations at densities below neutron drip (4 1011 g cm-3). We present results for the final element abundance distribution with and without heating from nuclear reactions, and compare to the solar abundance pattern of r-process elements. We highlight the distinguishing features of quark-novae by contrasting it with conventional nucleosynthetic sites such as type II supernovae and neutron star mergers, especially in the context of heavy-element compositions of extremely metal-deficient stars.
Key words: dense matter / nuclear reactions, nucleosynthesis, abundances / stars: neutron
© ESO, 2007
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