Numerical relativity simulations of prompt collapse mergers: Threshold mass and phenomenological constraints on neutron star properties after GW170817
Abstract
We determine the threshold mass for prompt (no bounce) black hole formation in equal-mass neutron star (NS) mergers using a new set of 227 numerical relativity simulations. We consider 23 phenomenological and microphysical finite-temperature equations of state (EOS), including models with hyperons and first-order phase transitions to deconfined quarks. We confirm the existence of EOS-insensitive relations between the threshold mass, binary tidal parameter at the threshold (Λth), maximum mass of nonrotating NSs, and radii of reference mass NSs. We combine the EOS-insensitive relations, phenomenological constraints on NS properties, and observational data from GW170817 to derive an improved lower limit on radii of maximum mass and a 1.6 M⊙ NS of 9.81 and 10.90 km, respectively. We also constrain the radius and quadrupolar tidal deformability (Λ) of a 1.4 M⊙ NS to be larger than 10.74 km and 172, respectively. We consider uncertainties in all independent parameters—fitting coefficients as well as GW170817 masses while reporting the range of radii constraints. We discuss an approach to constrain the upper as well as lower limit of NS maximum mass using future binary NS detections and their identification as prompt or delayed collapse. With future observations, it will be possible to derive even tightermore »
- Authors:
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[1];
[1];
[1];
[1];
[1];
[2];
[3];
[1];
[4];
[2];
[5];
[6];
[7]
- Pennsylvania State Univ., University Park, PA (United States)
- Univ. di Pisa (Italy); National Institute of Nuclear Physics (INFN), Pisa (Italy)
- Univ. di Trento (Italy); Istituto Nazionale di Fisica Nucleare, Trento (Italy). Trento Institute for Fundamental Physics and Applications (INFN-TIFPA)
- Friedrich Schiller Univ., Jena (Germany)
- Manhattan College, Riverdale, NY (United States)
- Indiana Univ., Bloomington, IN (United States)
- Stockholm Univ. (Sweden)
- Publication Date:
- Research Org.:
- Pennsylvania State Univ., University Park, PA (United States); Univ. of California, Oakland, CA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF)
- OSTI Identifier:
- 1980085
- Grant/Contract Number:
- SC0021177; AC02-05CH11231; PHY-2011725; PHY-2020275; PHY-2116686; AST-2108467
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review. D.
- Additional Journal Information:
- Journal Volume: 105; Journal Issue: 10; Journal ID: ISSN 2470-0010
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Physics; fluids & classical fields in curved spacetime; gravitational wave sources
Citation Formats
Kashyap, Rahul, Das, Abhishek, Radice, David, Padamata, Surendra, Prakash, Aviral, Logoteta, Domenico, Perego, Albino, Godzieba, Daniel A., Bernuzzi, Sebastiano, Bombaci, Ignazio, Fattoyev, Farrukh J., Reed, Brendan T., and Schneider, André Silva. Numerical relativity simulations of prompt collapse mergers: Threshold mass and phenomenological constraints on neutron star properties after GW170817. United States: N. p., 2022.
Web. doi:10.1103/physrevd.105.103022.
Kashyap, Rahul, Das, Abhishek, Radice, David, Padamata, Surendra, Prakash, Aviral, Logoteta, Domenico, Perego, Albino, Godzieba, Daniel A., Bernuzzi, Sebastiano, Bombaci, Ignazio, Fattoyev, Farrukh J., Reed, Brendan T., & Schneider, André Silva. Numerical relativity simulations of prompt collapse mergers: Threshold mass and phenomenological constraints on neutron star properties after GW170817. United States. https://doi.org/10.1103/physrevd.105.103022
Kashyap, Rahul, Das, Abhishek, Radice, David, Padamata, Surendra, Prakash, Aviral, Logoteta, Domenico, Perego, Albino, Godzieba, Daniel A., Bernuzzi, Sebastiano, Bombaci, Ignazio, Fattoyev, Farrukh J., Reed, Brendan T., and Schneider, André Silva. Fri .
"Numerical relativity simulations of prompt collapse mergers: Threshold mass and phenomenological constraints on neutron star properties after GW170817". United States. https://doi.org/10.1103/physrevd.105.103022. https://www.osti.gov/servlets/purl/1980085.
@article{osti_1980085,
title = {Numerical relativity simulations of prompt collapse mergers: Threshold mass and phenomenological constraints on neutron star properties after GW170817},
author = {Kashyap, Rahul and Das, Abhishek and Radice, David and Padamata, Surendra and Prakash, Aviral and Logoteta, Domenico and Perego, Albino and Godzieba, Daniel A. and Bernuzzi, Sebastiano and Bombaci, Ignazio and Fattoyev, Farrukh J. and Reed, Brendan T. and Schneider, André Silva},
abstractNote = {We determine the threshold mass for prompt (no bounce) black hole formation in equal-mass neutron star (NS) mergers using a new set of 227 numerical relativity simulations. We consider 23 phenomenological and microphysical finite-temperature equations of state (EOS), including models with hyperons and first-order phase transitions to deconfined quarks. We confirm the existence of EOS-insensitive relations between the threshold mass, binary tidal parameter at the threshold (Λth), maximum mass of nonrotating NSs, and radii of reference mass NSs. We combine the EOS-insensitive relations, phenomenological constraints on NS properties, and observational data from GW170817 to derive an improved lower limit on radii of maximum mass and a 1.6 M⊙ NS of 9.81 and 10.90 km, respectively. We also constrain the radius and quadrupolar tidal deformability (Λ) of a 1.4 M⊙ NS to be larger than 10.74 km and 172, respectively. We consider uncertainties in all independent parameters—fitting coefficients as well as GW170817 masses while reporting the range of radii constraints. We discuss an approach to constrain the upper as well as lower limit of NS maximum mass using future binary NS detections and their identification as prompt or delayed collapse. With future observations, it will be possible to derive even tighter constraints on the properties of matter at and above nuclear density using the method proposed in this work.},
doi = {10.1103/physrevd.105.103022},
journal = {Physical Review. D.},
number = 10,
volume = 105,
place = {United States},
year = {Fri May 20 00:00:00 EDT 2022},
month = {Fri May 20 00:00:00 EDT 2022}
}
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