Nucleosynthesis in neutron-rich ejecta from quark-novae

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dc.creatorJaikumar, Prashanth
dc.creatorMeyer, Bradley S.
dc.creatorOtsuki, Kaori
dc.creatorOuyed, Rachid
dc.date2006-10-04
dc.date2007-08-20
dc.date.accessioned2026-07-07T12:53:49Z
dc.date.available2026-07-07T12:53:49Z
dc.descriptionWe 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) < (Z,A) < (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 (n-gamma) equilibrium r-process calculations during the initially cold decompression phase. They match to dynamical r-process calculations at densities below neutron drip (4.10^11 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.
dc.descriptionjournal version; contains additional figure, sub-sections and references
dc.identifierhttps://arxiv.org/abs/nucl-th/0610013
dc.identifierhttp://arxiv.org/abs/nucl-th/0610013
dc.identifierAstron.Astrophys.471:227-236,2007
dc.identifierdoi:10.1051/0004-6361:20066593
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/223752
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.titleNucleosynthesis in neutron-rich ejecta from quark-novae
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