A Broad Grid of 2D Kilonova Emission Models

Wollaeger, Ryan Thomas; Fryer, Christopher Lee; Chase, Eve Adde; Fontes, Christopher John; Ristic, Marko; Hungerford, Aimee L.; Korobkin, Oleg; O'Shaughnessy, R.; Herring, Angela M.

doi:10.3847/1538-4357/ac0d03

A Broad Grid of 2D Kilonova Emission Models

Journal Article · Mon Aug 30 00:00:00 EDT 2021 · The Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/ac0d03· OSTI ID:1873330

^[1]; ^[2]; ^[3]; ^[1]; Ristic, Marko ^[4]; ^[5]; ^[5]; O'Shaughnessy, R. ^[6]; Herring, Angela M. ^[1]

Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Univ. of Arizona, Tucson, AZ (United States); Univ. of New Mexico, Albuquerque, NM (United States); George Washington Univ., Washington, DC (United States)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Northwestern Univ., Evanston, IL (United States)
Rochester Inst. of Technology, Rochester, NY (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements, Notre Dame, IN (United States)
Rochester Inst. of Technology, Rochester, NY (United States)

Depending upon the properties of their compact remnants and the physics included in the models, simulations of neutron star mergers can produce a broad range of ejecta properties. The characteristics of this ejecta, in turn, define the kilonova emission. To explore the effect of ejecta properties, we present a grid of 2-component 2D axisymmetric kilonova simulations that vary mass, velocity, morphology, and composition. The masses and velocities of each component vary, respectively, from 0.001 to 0.1 M_⊙ and 0.05 to 0.3c, covering much of the range of results from the neutron star merger literature. The set of 900 models is constrained to have a toroidal low electron fraction (Y_e) ejecta with a robust r-process composition and either a spherical or lobed high-Y_e ejecta with two possible compositions. We simulate these models with the Monte Carlo radiative transfer code SuperNu using a full suite of lanthanide and 4th row element opacities. We examine the trends of these models with parameter variation, show how it can be used with statistical tools, and compare the model light curves and spectra to those of AT2017gfo, the electromagnetic counterpart of GW170817.

View Accepted Manuscript (DOE)

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

Sponsoring Organization:: National Science Foundation (NSF); USDOE Laboratory Directed Research and Development (LDRD) Program

Grant/Contract Number:: 89233218CNA000001

OSTI ID:: 1873330

Alternate ID(s):: OSTI ID: 23158680

Report Number(s):: LA-UR-20-30338

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 1 Vol. 918; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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