r -process nucleosynthesis and kilonovae from hypermassive neutron star post-merger remnants

Curtis, Sanjana; Mösta, Philipp; Wu, Zhenyu; Radice, David; Roberts, Luke; Ricigliano, Giacomo; Perego, Albino

doi:10.1093/mnras/stac3128

Title: r -process nucleosynthesis and kilonovae from hypermassive neutron star post-merger remnants

Journal Article · Fri Nov 04 00:00:00 EDT 2022 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stac3128· OSTI ID:1903400

; Mösta, Philipp;

;

; Roberts, Luke;

; Perego, Albino

ABSTRACT We investigate r-process nucleosynthesis and kilonova emission resulting from binary neutron star (BNS) mergers based on a three-dimensional (3D) general-relativistic magnetohydrodynamic (GRMHD) simulation of a hypermassive neutron star (HMNS) remnant. The simulation includes a microphysical finite-temperature equation of state (EOS) and neutrino emission and absorption effects via a leakage scheme. We track the thermodynamic properties of the ejecta using Lagrangian tracer particles and determine its composition using the nuclear reaction network SkyNet. We investigate the impact of neutrinos on the nucleosynthetic yields by varying the neutrino luminosities during post-processing. The ejecta show a broad distribution with respect to their electron fraction Ye, peaking between ∼0.25–0.4 depending on the neutrino luminosity employed. We find that the resulting r-process abundance patterns differ from solar, with no significant production of material beyond the second r-process peak when using luminosities recorded by the tracer particles. We also map the HMNS outflows to the radiation hydrodynamics code SNEC and predict the evolution of the bolometric luminosity as well as broadband light curves of the kilonova. The bolometric light curve peaks on the timescale of a day and the brightest emission is seen in the infrared bands. This is the first direct calculation of the r-process yields and kilonova signal expected from HMNS winds based on 3D GRMHD simulations. For longer-lived remnants, these winds may be the dominant ejecta component producing the kilonova emission.

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Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA); USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF)

Grant/Contract Number:: 89233218CNA000001; SC0021177; PHY-2011725; PHY-2020275; PHY-2116686; AST2108467

OSTI ID:: 1903400

Alternate ID(s):: OSTI ID: 2315649

Report Number(s):: LA-UR-21-31691

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Vol. 518 Journal Issue: 4; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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