The influence of neutrinos on r-process nucleosynthesis in the ejecta of black hole–neutron star mergers

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dc.citation.epage3019en_US
dc.citation.issue4en_US
dc.citation.spage3907en_US
dc.citation.volume464en_US
dc.contributor.authorRoberts, Luke F.
dc.contributor.authorLippuner, Jonas
dc.contributor.authorDuez, Matthew D.
dc.contributor.authorFaber, Joshua A.
dc.contributor.authorFoucart, Francois
dc.contributor.authorLombardi, James C., Jr. (Jamie)
dc.contributor.authorNing, Sandra
dc.contributor.authorOtt, Christian D.
dc.contributor.authorPonce, Marcelo
dc.contributor.avlauthorLombardi, James C., Jr. (Jamie)
dc.contributor.departmentPhysicsen_US
dc.date.accessioned2017-04-10T14:16:04Z
dc.date.available2017-04-10T14:16:04Z
dc.date.issued2016-10-12
dc.description.abstractDuring the merger of a black hole and a neutron star, baryonic mass can become unbound from the system. Because the ejected material is extremely neutron-rich, the r-process rapidly synthesizes heavy nuclides as the material expands and cools. In this work, we map general relativistic models of black hole–neutron star mergers into a Newtonian smoothed particle hydrodynamics (SPH) code and follow the evolution of the thermodynamics and morphology of the ejecta until the outflows become homologous. We investigate how the subsequent evolution depends on our mapping procedure and find that the results are robust. Using thermodynamic histories from the SPH particles, we then calculate the expected nucleosynthesis in these outflows while varying the level of neutrino irradiation coming from the post-merger accretion disc. We find that the ejected material robustly produces r-process nucleosynthesis even for unrealistically high neutrino luminosities, due to the rapid velocities of the outflow. None the less, we find that neutrinos can have an impact on the detailed pattern of the r-process nucleosynthesis. Electron neutrinos are captured by neutrons to produce protons while neutron capture is occurring. The produced protons rapidly form low-mass seed nuclei for the r-process. These low-mass seeds are eventually incorporated into the first r-process peak at A ∼ 78. We consider the mechanism of this process in detail and discuss if it can impact galactic chemical evolution of the first peak r-process nuclei.en_US
dc.description.sponsorshipNational Aeronautics and Space Administration (NASA)- Chandra X-ray Center National Science Foundation (NSF) Sherman Fairchild Foundationen_US
dc.description.versionPublished articleen_US
dc.identifier.citationRoberts, L.F., Lippuner, J. Duez, M.D. et al. (2017). The influence of neutrinos on r-process nucleosynthesis in the ejecta of black hole-neutron star mergers. Monthly Notices of the Royal Astronomical Society 464(4): 3907-3919. Doi:10.1093/mnras/stw2622en_US
dc.identifier.doi10.1093/mnras/stw2622
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.urihttp://hdl.handle.net/10456/42627
dc.language.isoen_USen_US
dc.publisherOxford University Pressen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.relation.isversionofhttps://doi.org/10.1093/mnras/stw2622en_US
dc.rightsThis article is published and view-able. Copyright is retained by publisher. Contact the author or publisher for further use of this material.en_US
dc.subjecthydrodynamicsen_US
dc.subjectneutrinosen_US
dc.subjectnuclear reactionsen_US
dc.subjectnucleosynthesisen_US
dc.subjectabundancesen_US
dc.subjectstars: neutronen_US
dc.titleThe influence of neutrinos on r-process nucleosynthesis in the ejecta of black hole–neutron star mergersen_US
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