TY - JOUR
T1 - Binary neutron star merger simulations with a calibrated turbulence model
AU - Radice, David
N1 - Funding Information:
This research used the resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Simulations were also performed on the supercomputers Comet and Stampede (NSF XSEDE allocation TG-PHY160025), on NSF/NCSA Blue Waters (NSF AWD-1811236), and on the Advanced Computer Infrastructure (ACI) of the Institute for Computational and Data Science (ICDS) at Pennsylvania State University. It is a pleasure to thank S. Bernuzzi for discussions that motivated this work, A. Prakash for carefully proofreading the manuscript, L. Weih and L. Rezzolla for discussions, and S. Hild for the ET-D noise curve data.
Funding Information:
Funding: This research used the resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Simulations were also performed on the supercomputers Comet and Stampede (NSF XSEDE allocation TG-PHY160025), on NSF/NCSA Blue Waters (NSF AWD-1811236), and on the Advanced Computer Infrastructure (ACI) of the Institute for Computational and Data Science (ICDS) at Pennsylvania State University.
Publisher Copyright:
© 2020 by the authors.
PY - 2020/8
Y1 - 2020/8
N2 - Magnetohydrodynamic (MHD) turbulence in neutron star (NS) merger remnants can impact their evolution and multi-messenger signatures, complicating the interpretation of present and future observations. Due to the high Reynolds numbers and the large computational costs of numerical relativity simulations, resolving all the relevant scales of the turbulence will be impossible for the foreseeable future. Here, we adopt a method to include subgrid-scale turbulence in moderate resolution simulations by extending the large-eddy simulation (LES) method to general relativity (GR). We calibrate our subgrid turbulence model with results from very-high-resolution GRMHD simulations, and we use it to perform NS merger simulations and study the impact of turbulence. We find that turbulence has a quantitative, but not qualitative, impact on the evolution of NS merger remnants, on their gravitational wave signatures, and on the outflows generated in binary NS mergers. Our approach provides a viable path to quantify uncertainties due to turbulence in NS mergers.
AB - Magnetohydrodynamic (MHD) turbulence in neutron star (NS) merger remnants can impact their evolution and multi-messenger signatures, complicating the interpretation of present and future observations. Due to the high Reynolds numbers and the large computational costs of numerical relativity simulations, resolving all the relevant scales of the turbulence will be impossible for the foreseeable future. Here, we adopt a method to include subgrid-scale turbulence in moderate resolution simulations by extending the large-eddy simulation (LES) method to general relativity (GR). We calibrate our subgrid turbulence model with results from very-high-resolution GRMHD simulations, and we use it to perform NS merger simulations and study the impact of turbulence. We find that turbulence has a quantitative, but not qualitative, impact on the evolution of NS merger remnants, on their gravitational wave signatures, and on the outflows generated in binary NS mergers. Our approach provides a viable path to quantify uncertainties due to turbulence in NS mergers.
UR - http://www.scopus.com/inward/record.url?scp=85089512244&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85089512244&partnerID=8YFLogxK
U2 - 10.3390/SYM12081249
DO - 10.3390/SYM12081249
M3 - Article
AN - SCOPUS:85089512244
SN - 2073-8994
VL - 12
JO - Symmetry
JF - Symmetry
IS - 8
M1 - 1249
ER -