TY - JOUR
T1 - Magnetohydrodynamic Simulations of Self-Consistent Rotating Neutron Stars with Mixed Poloidal and Toroidal Magnetic Fields
AU - Tsokaros, Antonios
AU - Ruiz, Milton
AU - Shapiro, Stuart L.
AU - Uryū, Kōji
N1 - We thank the Illinois Relativity REU team (H. Jinghan, M. Kotak, E. Yu, and J. Zhou) for assistance with some of the visualizations. This work has been supported in part by National Science Foundation (NSF) Grant No. PHY-2006066, and NASA Grant No. 80NSSC17K0070 to the University of Illinois at Urbana-Champaign, as well as by JSPS Grant-in-Aid for Scientific Research(C) 18K03624 to the University of the Ryukyus. 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 (Awards 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. Resources supporting this work were also provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. This research is part of the Frontera computing project at the Texas Advanced Computing Center. Frontera is made possible by National Science Foundation Award No. OAC-1818253.
PY - 2022/2/11
Y1 - 2022/2/11
N2 - We perform the first magnetohydrodynamic simulations in full general relativity of self-consistent rotating neutron stars (NSs) with ultrastrong mixed poloidal and toroidal magnetic fields. The initial uniformly rotating NS models are computed assuming perfect conductivity, stationarity, and axisymmetry. Although the specific geometry of the mixed field configuration can delay or accelerate the development of various instabilities known from analytic perturbative studies, all our models finally succumb to them. Differential rotation is developed spontaneously in the cores of our magnetars which, after sufficient time, is converted back to uniform rotation. The rapidly rotating magnetars show a significant amount of ejecta, which can be responsible for transient kilonova signatures. However, no highly collimated, helical magnetic fields or incipient jets, which are necessary for γ-ray bursts, arise at the poles of these magnetars by the time our simulations are terminated.
AB - We perform the first magnetohydrodynamic simulations in full general relativity of self-consistent rotating neutron stars (NSs) with ultrastrong mixed poloidal and toroidal magnetic fields. The initial uniformly rotating NS models are computed assuming perfect conductivity, stationarity, and axisymmetry. Although the specific geometry of the mixed field configuration can delay or accelerate the development of various instabilities known from analytic perturbative studies, all our models finally succumb to them. Differential rotation is developed spontaneously in the cores of our magnetars which, after sufficient time, is converted back to uniform rotation. The rapidly rotating magnetars show a significant amount of ejecta, which can be responsible for transient kilonova signatures. However, no highly collimated, helical magnetic fields or incipient jets, which are necessary for γ-ray bursts, arise at the poles of these magnetars by the time our simulations are terminated.
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U2 - 10.1103/PhysRevLett.128.061101
DO - 10.1103/PhysRevLett.128.061101
M3 - Article
C2 - 35213191
AN - SCOPUS:85124973730
SN - 0031-9007
VL - 128
JO - Physical review letters
JF - Physical review letters
IS - 6
M1 - 061101
ER -