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We present an analytic, perturbative solution that describes dynamical black holes in a slowroll inflationary cosmology. It is shown that the metric evolves quasistatically through a sequence of quasiSchwarzchilddeSitter metrics with time dependent cosmological constant and mass parameters, such that the cosmological constant is instantaneously equal to the value of the scalar potential. The areas of the black hole and cosmological horizons each increase in time as the effective cosmological constant decreases, and the the factional area increase is proportional to the fractional change of the cosmological constant, times a geometrical factor. For black holes ranging in size from much smaller than to comparable to the cosmological horizon, the prefactor varies from very small to order one. The change in the horizon areas happens in such a way that the first laws of thermodynamics are satisfied throughout the evolution.
\n\nSPEAKER: Jennie Tracshen, University of Massachusetts at Amherst 464 Loomis false
Mathematical and Theoretical Physics Seminar: "University of Massachusetts at Amherst"
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Jennie Tracshen, University of Massachusetts at Amherst 

Date:  12/6/2018 
Time:  12:30 p.m. 
Location:  464 Loomis 
Sponsor:  Physics Department 
Event Type:  Seminar/Symposium 
We present an analytic, perturbative solution that describes dynamical black holes in a slowroll inflationary cosmology. It is shown that the metric evolves quasistatically through a sequence of quasiSchwarzchilddeSitter metrics with time dependent cosmological constant and mass parameters, such that the cosmological constant is instantaneously equal to the value of the scalar potential. The areas of the black hole and cosmological horizons each increase in time as the effective cosmological constant decreases, and the the factional area increase is proportional to the fractional change of the cosmological constant, times a geometrical factor. For black holes ranging in size from much smaller than to comparable to the cosmological horizon, the prefactor varies from very small to order one. The change in the horizon areas happens in such a way that the first laws of thermodynamics are satisfied throughout the evolution.

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