TY - JOUR
T1 - Gravitational wave content and stability of uniformly, rotating, triaxial neutron stars in general relativity
AU - Tsokaros, Antonios
AU - Ruiz, Milton
AU - Paschalidis, Vasileios
AU - Shapiro, Stuart L.
AU - Baiotti, Luca
AU - Uryū, Kōji
N1 - Funding Information:
This work was supported by NSF Grants No. PHY-1300903, No. PHY-1602536, and No. PHY-1607449; NASA Grants No. NNX13AH44G and No. NNX16AR67G (Fermi); and JSPS Grants-in-Aid for Scientific Research (C), Grants No. 26400274 and No. 15K05085. V.P. gratefully acknowledges support from the Simons Foundation. This work made use of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. TG-MCA99S008. This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Grants No. OCI-0725070 and No. ACI-1238993) 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. Some numerical computations were carried out on the XC30 system at the Center for Computational Astrophysics of the National Astronomical Observatory of Japan.
Publisher Copyright:
© 2017 American Physical Society.
PY - 2017/6/15
Y1 - 2017/6/15
N2 - Targets for ground-based gravitational wave interferometers include continuous, quasiperiodic sources of gravitational radiation, such as isolated, spinning neutron stars. In this work, we perform evolution simulations of uniformly rotating, triaxially deformed stars, the compressible analogs in general relativity of incompressible, Newtonian Jacobi ellipsoids. We investigate their stability and gravitational wave emission. We employ five models, both normal and supramassive, and track their evolution with different grid setups and resolutions, as well as with two different evolution codes. We find that all models are dynamically stable and produce a strain that is approximately one-tenth the average value of a merging binary system. We track their secular evolution and find that all our stars evolve toward axisymmetry, maintaining their uniform rotation, rotational kinetic energy, and angular momentum profiles while losing their triaxiality.
AB - Targets for ground-based gravitational wave interferometers include continuous, quasiperiodic sources of gravitational radiation, such as isolated, spinning neutron stars. In this work, we perform evolution simulations of uniformly rotating, triaxially deformed stars, the compressible analogs in general relativity of incompressible, Newtonian Jacobi ellipsoids. We investigate their stability and gravitational wave emission. We employ five models, both normal and supramassive, and track their evolution with different grid setups and resolutions, as well as with two different evolution codes. We find that all models are dynamically stable and produce a strain that is approximately one-tenth the average value of a merging binary system. We track their secular evolution and find that all our stars evolve toward axisymmetry, maintaining their uniform rotation, rotational kinetic energy, and angular momentum profiles while losing their triaxiality.
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U2 - 10.1103/PhysRevD.95.124057
DO - 10.1103/PhysRevD.95.124057
M3 - Article
AN - SCOPUS:85022345623
SN - 2470-0010
VL - 95
JO - Physical Review D
JF - Physical Review D
IS - 12
ER -