2019/06/25 by Koji Uryu, Kōji Uryū, Shijun Yoshida +8 · 36 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Classical mechanics #Compact space #Compact star #Cosmology and Gravitation Theories #Magnetic field #Magnetohydrodynamics #Mathematical analysis #Neutron star #Physics #Plasma #Pulsars and Gravitational Waves Research #Quantum mechanics #Stars #Toroid #astro-ph.HE #gr-qc
paper · pdf · doi:10.1103/physrevd.100.123019
published in Physical review. D/Physical review. D. 100(12) (American Physical Society) · 30 pages, 4 figures
arxiv created 2019/06/25 · openalex created_date 2019/07/12 · openalex publication_date 2019/12/19 · arxiv updated 2019/12/25 · openalex updated_date 2026/08/06
A new code for computing fully general relativistic solutions of strongly magnetized rapidly rotating compact stars is developed as a part of the Compact Object CALculator (cocal) code. The full set of Einstein's equations, Maxwell's equations, and magnetohydrodynamic equations are consistently solved assuming perfect conductivity, stationarity, and axisymmetry, and strongly magnetized solutions associated with mixed poloidal and toroidal components of magnetic fields are successfully obtained in generic (noncircular) spacetimes. We introduce the formulation of the problem and the numerical method in detail, then present examples of extremely magnetized compact star solutions and their convergence tests. It is found that, in extremely magnetized stars, the stellar matter can be expelled from the region of strongest toroidal fields. Hence, we conjecture that a toroidal electrovacuum region may appear inside of the extremely magnetized compact stars, which may seem like the neutron star becoming the strongest toroidal solenoid coil in the Universe.