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SUMMARY:Thermodynamic instability of rotating black holes - Ricardo Montei
 ro (DAMTP\, Cambridge)
DTSTART:20090220T130000Z
DTEND:20090220T140000Z
UID:TALK16538@talks.cam.ac.uk
CONTACT:Dr H K Kunduri
DESCRIPTION:We show that the quasi-Euclidean sections of various rotating 
 black holes in\ndifferent dimensions possess at least one non-conformal ne
 gative mode when\nthermodynamic instabilities are expected. The boundary c
 onditions of fixed\ninduced metric correspond to the partition function of
  the grand canonical\nensemble. Indeed\, in the asymptotically flat cases\
 , we find that a negative\nmode persists even if the specific heat at cons
 tant angular momenta is\npositive\, since the stability in this ensemble a
 lso requires the positivity\nof the isothermal momentum of inertia. We foc
 us in particular on Kerr black\nholes\, on Myers-Perry black holes in five
  and six dimensions\, and on the\nEmparan-Reall black ring solution. We go
  on further to consider the richer\ncase of the asymptotically AdS Kerr bl
 ack hole in four dimensions\, where\nthermodynamic stability is expected f
 or a large enough cosmological\nconstant. The results are consistent with 
 previous findings in the\nnon-rotation limit and support the use of quasi-
 Euclidean instantons to\nconstruct gravitational partition functions.
LOCATION:Pavilion B Potter Room (B1.19)
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