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Title: Impact of Pulsar and Fallback Sources on Multifrequency Kilonova Models

Abstract

We explore the impact of pulsar electromagnetic dipole and fallback accretion emission on the luminosity of a suite of kilonova models. The pulsar models are varied over pulsar magnetic field strength, pulsar lifetime, ejecta mass, and elemental abundances; the fallback models are varied over fallback accretion rate and ejecta mass. For the abundances, we use Fe and Nd as representatives of the wind and dynamical ejecta, respectively. We simulate radiative transfer in the ejecta in either 1D spherical or 2D cylindrical spatial geometry. For the grid of 1D simulations, the mass fraction of Nd is 0, 10 –4, or 10 –3, and the rest is Fe. Our models that fit the bolometric luminosity of AT 2017gfo (the kilonova associated with the first neutron star merger discovered in gravitational waves, GW170817) do not simultaneously fit the B, V, and I time evolution. Here, we find that the trends of the evolution in B and V magnitudes are better matched by the fallback model relative to the pulsar model, implying the time-dependence of the remnant source influences the color evolution. Further exploration of the parameter space and model deficiencies is needed before we can describe AT 2017gfo with a remnant source.

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [1]; ORCiD logo [1]; ORCiD logo [1]; ORCiD logo [3]; ORCiD logo [3]; ORCiD logo [1]; ORCiD logo [1]
  1. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  2. Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements, East Lansing, MI (United States); The George Washington Univ., Washington, DC (United States)
  3. Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements, East Lansing, MI (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Laboratory Directed Research and Development (LDRD) Program
OSTI Identifier:
1565901
Report Number(s):
LA-UR-19-22590
Journal ID: ISSN 1538-4357
Grant/Contract Number:  
89233218CNA000001
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 880; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; methods: numerical; radiative transfer; stars: neutron; supernovae: general

Citation Formats

Wollaeger, Ryan Thomas, Fryer, Chris Lee, Fontes, Christopher John, Lippuner, Jonas, Vestrand, W. Thomas, Mumpower, Matthew Ryan, Korobkin, Oleg, Hungerford, Aimee L., and Even, Wesley Paul. Impact of Pulsar and Fallback Sources on Multifrequency Kilonova Models. United States: N. p., 2019. Web. doi:10.3847/1538-4357/ab25f5.
Wollaeger, Ryan Thomas, Fryer, Chris Lee, Fontes, Christopher John, Lippuner, Jonas, Vestrand, W. Thomas, Mumpower, Matthew Ryan, Korobkin, Oleg, Hungerford, Aimee L., & Even, Wesley Paul. Impact of Pulsar and Fallback Sources on Multifrequency Kilonova Models. United States. doi:10.3847/1538-4357/ab25f5.
Wollaeger, Ryan Thomas, Fryer, Chris Lee, Fontes, Christopher John, Lippuner, Jonas, Vestrand, W. Thomas, Mumpower, Matthew Ryan, Korobkin, Oleg, Hungerford, Aimee L., and Even, Wesley Paul. Fri . "Impact of Pulsar and Fallback Sources on Multifrequency Kilonova Models". United States. doi:10.3847/1538-4357/ab25f5.
@article{osti_1565901,
title = {Impact of Pulsar and Fallback Sources on Multifrequency Kilonova Models},
author = {Wollaeger, Ryan Thomas and Fryer, Chris Lee and Fontes, Christopher John and Lippuner, Jonas and Vestrand, W. Thomas and Mumpower, Matthew Ryan and Korobkin, Oleg and Hungerford, Aimee L. and Even, Wesley Paul},
abstractNote = {We explore the impact of pulsar electromagnetic dipole and fallback accretion emission on the luminosity of a suite of kilonova models. The pulsar models are varied over pulsar magnetic field strength, pulsar lifetime, ejecta mass, and elemental abundances; the fallback models are varied over fallback accretion rate and ejecta mass. For the abundances, we use Fe and Nd as representatives of the wind and dynamical ejecta, respectively. We simulate radiative transfer in the ejecta in either 1D spherical or 2D cylindrical spatial geometry. For the grid of 1D simulations, the mass fraction of Nd is 0, 10–4, or 10–3, and the rest is Fe. Our models that fit the bolometric luminosity of AT 2017gfo (the kilonova associated with the first neutron star merger discovered in gravitational waves, GW170817) do not simultaneously fit the B, V, and I time evolution. Here, we find that the trends of the evolution in B and V magnitudes are better matched by the fallback model relative to the pulsar model, implying the time-dependence of the remnant source influences the color evolution. Further exploration of the parameter space and model deficiencies is needed before we can describe AT 2017gfo with a remnant source.},
doi = {10.3847/1538-4357/ab25f5},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 880,
place = {United States},
year = {2019},
month = {7}
}

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