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Add to Calendar 12/6/2018 12:30 pm 12/6/2018 America/Chicago Mathematical and Theoretical Physics Seminar: "University of Massachusetts at Amherst" DESCRIPTION:

We present an analytic, perturbative solution that describes dynamical black holes in a slow-roll inflationary cosmology.  It is shown that the metric evolves quasi-statically through a sequence of quasi-Schwarzchild-deSitter 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 pre-factor 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

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Mathematical and Theoretical Physics Seminar: "University of Massachusetts at Amherst"

Speaker 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 slow-roll inflationary cosmology.  It is shown that the metric evolves quasi-statically through a sequence of quasi-Schwarzchild-deSitter 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 pre-factor 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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