The Meissner effect for weakly isolated horizons

Abstract

Black holes are important astrophysical objects describing an end state of stellar evolution, which are observed frequently. There are theoretical predictions that Kerr black holes with high spins expel magnetic fields. However, Kerr black holes are pure vacuum solutions, which do not include accretion disks, and additionally previous investigations are mainly limited to weak magnetic fields. We prove for the first time in full general relativity that generic rapidly spinning black holes including those deformed by accretion disks still expel even strong magnetic fields. Analogously to a similar property of superconductors, this is called Meissner effect.

7 pages, 4 figures

References in corpus (6)

• No-hair theorem for Black Holes in Astrophysical Environments
• "Meissner effect" and Blandford-Znajek mechanism in conductive black hole magnetospheres
• Reflection From the Strong Gravity Regime in a z=0.658 Gravitationally Lensed-Quasar
• The Black Hole Meissner Effect and Blandford-Znajek Jets
• Black hole Meissner effect and entanglement
• Neighbourhoods of Isolated Horizons and their stationarity

Cited by in corpus (7)

• Resonance crossing of a charged body in a magnetized Kerr background: an analogue of extreme mass ratio inspiral
• On Beltrami states near black hole event horizon
• Kerr-Newman black hole in the formalism of isolated horizons
• Black hole in a superconducting plasma
• Extremal isolated horizons with $\Lambda$ and the related unique type D black holes
• Zooming in on the horizon when in its Meissner state
• Initial data for a deformed isolated horizon