Neutron reactions in accreting neutron stars: a new pathway to efficient crust heating

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dc.creatorGupta, Sanjib S.
dc.creatorKawano, Toshihiko
dc.creatorMöller, Peter
dc.date2008-11-11
dc.date.accessioned2026-07-07T12:15:59Z
dc.date.available2026-07-07T12:15:59Z
dc.descriptionIn our calculation of neutron star crust heating we include several key new model features. In earlier work electron capture (EC) only allowed neutron emission from the daughter ground-state; here we calculate, in a deformed QRPA model, EC decay rates to all states in the daughter that are allowed by Gamow-Teller selection rules and energetics. The subsequent branching ratios between the 1n,...,xn channels and the competing $γ$-decay are calculated in a Hauser-Feshbach model. Since EC accesses excited states, many more neutrons are emitted in our calculation than in previous work, leading to accelerated reaction flows. In our multi-component plasma model a single (EC,xn) reaction step can produce several neutron-deficient nuclei, each of which can further decay by (EC,xn). Hence, the neutron emission occurs more continuously with increasing depth as compared to that in a one-component plasma model.
dc.descriptionTwo color figures, accepted for publication by Physical Review Letters
dc.identifierhttps://arxiv.org/abs/0811.1791
dc.identifierhttp://arxiv.org/abs/0811.1791
dc.identifierPhys.Rev.Lett.101:231101,2008
dc.identifierdoi:10.1103/PhysRevLett.101.231101
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/211660
dc.subjectAstrophysics
dc.titleNeutron reactions in accreting neutron stars: a new pathway to efficient crust heating
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