期刊
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
卷 244, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4365/ab3922
关键词
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资金
- Interuniversity Attraction Poles Programme by the Belgian Science Policy Office [IAP P7/08 CHARM]
- ERC synergy grant BlackHoleCam: Imaging the Event Horizon of Black Holes [610058]
- Alexander von Humboldt Fellowship
- Research Foundation-Flanders (FWO) [12Q6117N]
- Flemish Government-department EWI
- Iboga cluster at the ITP Frankfurt
- Research Foundation Flanders (FWO)
- KU Leuven [GOA/2015-014]
Recent advances in black hole astrophysics, particularly the first visual evidence of a supermassive black hole at the center of the galaxy M87 by the Event Horizon Telescope, and the detection of an orbiting hot spot nearby the event horizon of Sgr A* in the Galactic center by the Gravity Collaboration, require the development of novel numerical methods to understand the underlying plasma microphysics. Non-thermal emission related to such hot spots is conjectured to originate from plasmoids that form due to magnetic reconnection in thin current layers in the innermost accretion zone. Resistivity plays a crucial role in current sheet formation, magnetic reconnection, and plasmoid growth in black hole accretion disks and jets. We included resistivity in the three-dimensional general-relativistic magnetohydrodynamics (GRMHD) code BHAC and present the implementation of an implicit-explicit scheme to treat the stiff resistive source terms of the GRMHD equations. The algorithm is tested in combination with adaptive mesh refinement to resolve the resistive scales and a constrained transport method to keep the magnetic field solenoidal. Several novel methods for primitive-variable recovery, a key part in relativistic magnetohydrodynamics codes, are presented and compared for accuracy, robustness, and efficiency. We propose a new inversion strategy that allows for resistive-GRMHD simulations of low gas-to-magnetic pressure ratio and highly magnetized regimes as applicable for black hole accretion disks, jets, and neutron-star magnetospheres. We apply the new scheme to study the effect of resistivity on accreting black holes, accounting for dissipative effects as reconnection.
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