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Title: Predicting spectra and lightcurves of macronovae, the electromagnetic signatures of the r-process nucleosynthesis

Authors:
ORCiD logo [1]; ORCiD logo [1]; ORCiD logo [1];  [2]; ORCiD logo [1]; ORCiD logo [1];  [2]; ORCiD logo [1];  [3];  [1]
  1. Los Alamos National Laboratory
  2. The Oskar Klein Centre, Stockholm University, Albanova, Stockholm, Sweden
  3. Radboud Radio Lab, Radboud University, Netherlands
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:
1374283
Report Number(s):
LA-UR-17-24973
DOE Contract Number:
AC52-06NA25396
Resource Type:
Conference
Resource Relation:
Conference: The Physics of Extreme-Gravity Stars ; 2017-06-05 - 2017-06-30 ; Stockholm, Sweden
Country of Publication:
United States
Language:
English

Citation Formats

Korobkin, Oleg, Wollaeger, Ryan Thomas, Fontes, Christopher John, Rosswog, Stephan K., Even, Wesley Paul, Fryer, Christopher Lee, Sollerman, Jesper, Hungerford, Aimee L., van Rossum, Daniel R., and Wollaber, Allan Benton. Predicting spectra and lightcurves of macronovae, the electromagnetic signatures of the r-process nucleosynthesis. United States: N. p., 2017. Web.
Korobkin, Oleg, Wollaeger, Ryan Thomas, Fontes, Christopher John, Rosswog, Stephan K., Even, Wesley Paul, Fryer, Christopher Lee, Sollerman, Jesper, Hungerford, Aimee L., van Rossum, Daniel R., & Wollaber, Allan Benton. Predicting spectra and lightcurves of macronovae, the electromagnetic signatures of the r-process nucleosynthesis. United States.
Korobkin, Oleg, Wollaeger, Ryan Thomas, Fontes, Christopher John, Rosswog, Stephan K., Even, Wesley Paul, Fryer, Christopher Lee, Sollerman, Jesper, Hungerford, Aimee L., van Rossum, Daniel R., and Wollaber, Allan Benton. Mon . "Predicting spectra and lightcurves of macronovae, the electromagnetic signatures of the r-process nucleosynthesis". United States. doi:. https://www.osti.gov/servlets/purl/1374283.
@article{osti_1374283,
title = {Predicting spectra and lightcurves of macronovae, the electromagnetic signatures of the r-process nucleosynthesis},
author = {Korobkin, Oleg and Wollaeger, Ryan Thomas and Fontes, Christopher John and Rosswog, Stephan K. and Even, Wesley Paul and Fryer, Christopher Lee and Sollerman, Jesper and Hungerford, Aimee L. and van Rossum, Daniel R. and Wollaber, Allan Benton},
abstractNote = {},
doi = {},
journal = {},
number = ,
volume = ,
place = {United States},
year = {Mon Aug 07 00:00:00 EDT 2017},
month = {Mon Aug 07 00:00:00 EDT 2017}
}

Conference:
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  • We present a near-infrared spectral sequence of the electromagnetic counterpart to the binary neutron star merger GW170817 detected by Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo. Our data set comprises seven epochs of J + H spectra taken with FLAMINGOS-2 on Gemini-South between 1.5 and 10.5 days after the merger. In the initial epoch, the spectrum is dominated by a smooth blue continuum due to a high-velocity, lanthanide-poor blue kilonova component. Starting the following night, all of the subsequent spectra instead show features that are similar to those predicted in model spectra of material with a high concentration of lanthanides, includingmore » spectral peaks near 1.07 and 1.55 μ m. Our fiducial model with 0.04 M {sub ⊙} of ejecta, an ejection velocity of v = 0.1 c , and a lanthanide concentration of X {sub lan} = 10{sup −2} provides a good match to the spectra taken in the first five days, although it over-predicts the late-time fluxes. We also explore models with multiple fitting components, in each case finding that a significant abundance of lanthanide elements is necessary to match the broad spectral peaks that we observe starting at 2.5 days after the merger. These data provide direct evidence that binary neutron star mergers are significant production sites of even the heaviest r -process elements.« less
  • Here, we present a near-infrared spectral sequence of the electromagnetic counterpart to the binary neutron star merger GW170817 detected by Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo. Our data set comprises seven epochs of J+H spectra taken with FLAMINGOS-2 on Gemini-South between 1.5 and 10.5 days after the merger. In the initial epoch, the spectrum is dominated by a smooth blue continuum due to a high-velocity, lanthanide-poor blue kilonova component. Starting the following night, all of the subsequent spectra instead show features that are similar to those predicted in model spectra of material with a high concentration of lanthanides, including spectralmore » peaks near 1.07 and 1.55 μm. Our fiducial model with 0.04 M ⊙ of ejecta, an ejection velocity of v = 0.1c, and a lanthanide concentration of X lan = 10 –2 provides a good match to the spectra taken in the first five days, although it over-predicts the late-time fluxes. We also explore models with multiple fitting components, in each case finding that a significant abundance of lanthanide elements is necessary to match the broad spectral peaks that we observe starting at 2.5 days after the merger. These data provide direct evidence that binary neutron star mergers are significant production sites of even the heaviest r-process elements.« less
    Cited by 13
  • Here, we present a near-infrared spectral sequence of the electromagnetic counterpart to the binary neutron star merger GW170817 detected by Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo. Our data set comprises seven epochs of J+H spectra taken with FLAMINGOS-2 on Gemini-South between 1.5 and 10.5 days after the merger. In the initial epoch, the spectrum is dominated by a smooth blue continuum due to a high-velocity, lanthanide-poor blue kilonova component. Starting the following night, all of the subsequent spectra instead show features that are similar to those predicted in model spectra of material with a high concentration of lanthanides, including spectralmore » peaks near 1.07 and 1.55 μm. Our fiducial model with 0.04 M ⊙ of ejecta, an ejection velocity of v = 0.1c, and a lanthanide concentration of X lan = 10 –2 provides a good match to the spectra taken in the first five days, although it over-predicts the late-time fluxes. We also explore models with multiple fitting components, in each case finding that a significant abundance of lanthanide elements is necessary to match the broad spectral peaks that we observe starting at 2.5 days after the merger. These data provide direct evidence that binary neutron star mergers are significant production sites of even the heaviest r-process elements.« less
    Cited by 13