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SUMMARY:Linear stability of charged rotating black holes  - Damon Civin (C
 CA)
DTSTART:20131106T160000Z
DTEND:20131106T170000Z
UID:TALK46768@talks.cam.ac.uk
CONTACT:Marcus Webb
DESCRIPTION:The Einstein field equations (EFE) are the fundamental equatio
 ns of general relativity\, the accepted theory of gravity. Perhaps the mos
 t striking prediction of general relativity is the existence of black hole
 s – regions of spacetime where the gravitational field is so strong that
  nothing can escape.\nBlack holes are believed to be abundant in the unive
 rse\, forming when matter (such as a star or galaxy) undergoes gravitation
 al collapse. Once a black hole has formed\, it is expected to be stable. T
 hat is\, black holes should not be sensitive to the influence of other obj
 ects and phenomena – they are the final state of the system. Providing a
  mathematical proof of the stability of black holes is one of the most imp
 ortant open problems in general relativity.\n\nGreat progress has been mad
 e by considering the (EFE) as a system of quasilinear wave equations. In m
 y talk\, I will introduce this approach to the study of general relativity
 \, focusing on the linear stability of subextremal Kerr-Newman spacetimes.
  Each member of this family models a charged rotating black hole. The stab
 ility of this family of spacetimes is of special interest as it is closely
  related to the plausibility of the concept of a black hole. Time permitti
 ng\, I will discuss my recent results in this direction. 
LOCATION:MR14\, Centre for Mathematical Sciences
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