Abstract
Recent numerical simulations in general relativistic magnetohydrodynamics (GRMHD) provide useful constraints for the interpretation of the GW170817 discovery. Combining the observed data with these simulations leads to a bound on the maximum mass of a cold, spherical neutron star (the TOV limit): Mmaxsph≲2.74/β, where β is the ratio of the maximum mass of a uniformly rotating neutron star (the supramassive limit) over the maximum mass of a nonrotating star. Causality arguments allow β to be as high as 1.27, while most realistic candidate equations of state predict β to be closer to 1.2, yielding Mmaxsph in the range 2.16-2.28M⊙. A minimal set of assumptions based on these simulations distinguishes this analysis from previous ones, but leads a to similar estimate. There are caveats, however, and they are enumerated and discussed. The caveats can be removed by further simulations and analysis to firm up the basic argument.
| Original language | English (US) |
|---|---|
| Article number | 021501 |
| Journal | Physical Review D |
| Volume | 97 |
| Issue number | 2 |
| DOIs | |
| State | Published - Jan 11 2018 |
ASJC Scopus subject areas
- Physics and Astronomy (miscellaneous)
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GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass. / Ruiz, Milton; Shapiro, Stuart L.; Tsokaros, Antonios.
In: Physical Review D, Vol. 97, No. 2, 021501, 11.01.2018.Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass
AU - Ruiz, Milton
AU - Shapiro, Stuart L.
AU - Tsokaros, Antonios
N1 - Funding Information: It is a pleasure to thank G. Baym, C. Gammie, F. Lamb, V. Paschalidis, E. Zhou and K. Uryū for useful discussions. We also thank the Illinois Relativity group REU team, E. Connelly, J. Simone, I. Sultan and J. Zhu for assistance in creating Fig. 1 . This work has been supported in part by National Science Foundation (NSF) Grants No. PHY-1602536 and No. PHY-1662211, and NASA Grants No. NNX13AH44G and No. 80NSSC17K0070 at the University of Illinois at Urbana-Champaign. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF Grant No. OCI-1053575. This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Award No. OCI 07-25070) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. [1] 1 B. P. 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PY - 2018/1/11
Y1 - 2018/1/11
N2 - Recent numerical simulations in general relativistic magnetohydrodynamics (GRMHD) provide useful constraints for the interpretation of the GW170817 discovery. Combining the observed data with these simulations leads to a bound on the maximum mass of a cold, spherical neutron star (the TOV limit): Mmaxsph≲2.74/β, where β is the ratio of the maximum mass of a uniformly rotating neutron star (the supramassive limit) over the maximum mass of a nonrotating star. Causality arguments allow β to be as high as 1.27, while most realistic candidate equations of state predict β to be closer to 1.2, yielding Mmaxsph in the range 2.16-2.28M⊙. A minimal set of assumptions based on these simulations distinguishes this analysis from previous ones, but leads a to similar estimate. There are caveats, however, and they are enumerated and discussed. The caveats can be removed by further simulations and analysis to firm up the basic argument.
AB - Recent numerical simulations in general relativistic magnetohydrodynamics (GRMHD) provide useful constraints for the interpretation of the GW170817 discovery. Combining the observed data with these simulations leads to a bound on the maximum mass of a cold, spherical neutron star (the TOV limit): Mmaxsph≲2.74/β, where β is the ratio of the maximum mass of a uniformly rotating neutron star (the supramassive limit) over the maximum mass of a nonrotating star. Causality arguments allow β to be as high as 1.27, while most realistic candidate equations of state predict β to be closer to 1.2, yielding Mmaxsph in the range 2.16-2.28M⊙. A minimal set of assumptions based on these simulations distinguishes this analysis from previous ones, but leads a to similar estimate. There are caveats, however, and they are enumerated and discussed. The caveats can be removed by further simulations and analysis to firm up the basic argument.
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U2 - 10.1103/PhysRevD.97.021501
DO - 10.1103/PhysRevD.97.021501
M3 - Article
C2 - 30003183
AN - SCOPUS:85042026813
VL - 97
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 2
M1 - 021501
ER -