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Time: 11am
Place: DRL 4N12

Title: TBA
Time: 2pm
Place: DRL 2N36

Special Seminar
Title: TBA
Time: 2pm
Place: DRL 4N12

Time: 2 pm
Place: DRL 2N36

Time: 2 p.m.
Place: 4N12

Time: 2 pm
Place: DRL 2N36

Math-Physics Joint Seminar
Title: Singularities and phases of gauge theories
Time: 4:30 pm
Place: DRL 4E19

Abstract:
Motivated by M-theory compactification on elliptic Calabi-Yau threefolds, we present a correspondence between networks of small resolutions for singular elliptic fibrations and Coulomb branches of five-dimensional N=1 gauge theories. While resolutions correspond to subchambers of the Coulomb branch, partial resolutions correspond to higher codimension loci at which the Coulomb branch intersects the Coulomb-Higgs branches. Flops between different resolutions are identified with reflections on the Coulomb branch. Physics aside, this correspondence provides an interesting link between elliptic fibrations and representation theory.

Title: Galileons and inequivalent representations of spacetime symmetries
Time: 2 pm
Place: DRL 4N12

Title: Systematically classifying elliptically fibered Calabi-Yau threefolds and corresponding F-theory models
Time: 2pm
Place: DRL 2N36

Title: Issues in early universe cosmology
Time: 2 pm
Place: DRL 2N36

Title: On the Classification of 6D SCFTs
Time: 2 pm
Place: DRL 2N36

Title: Supergoop and the emergence of AdS_2
Time: 2 p.m.
Place: DRL 2N36
 

Title: Analytic structure of correlation functions in conformal field theories
Time: 2 p.m.
Place: DRL 2N36

Deformation Theory Seminar
Title: Towards Generalized Spacetimes in String and M-theory
Time: 2 pm  
Place: DRL 2C8

Title: Double and Exceptional Field Theory
Time: 2pm
Place: DRL 2N36
 
Abstract:
I review double field theory and recent progress in generalizing it to the
U-duality symmetries of M-theory. Specifically, I discuss extensions of 
11-dimensional supergravity and type IIB based on generalized spacetimes,
in which the exceptional groups E6 and E7 become manifest symmetries.

Time: 2 pm
Place: DRL 2N36
 
Stars and black holes in massive gravity
I will consider spherically symmetric solutions in an asymptotically flat universe with a massive graviton, and argue that: (a) For small graviton mass ($m$) Einstein gravity is recovered at small radii, as Vainshtein anticipated. (b) Static black holes, however, are singular at horizon, no matter how small is the graviton mass. (c) Analogously, static charged black holes have a horizon singularity in massive electrodynamics. In reality, they loose their electric field and discharge. (d) Black holes in massive gravity must also be time-dependent. Now they loose mass and gradually disappear. (e) The disappearance rate of a black hole with radius $r_g$ scales as $m^2 r_g$. Therefore, in the limit $m\to 0$ one recovers Einstein gravity.

Distributed SUSY Breaking: Technically Natural Vacuum Energy from 6D Supergravity

In this talk, I'll present an extra-dimensional brane-world model which breaks supersymmetry through a non-local condition: flux quantization. After reviewing the properties of a particular set of solutions to the bulk field equations -- and explaining why the 4D curvature vanishes at the classical level for these solutions -- I'll demonstrate that the leading-order quantum corrections to the vacuum energy are technically natural, and have a size set by the Kaluza-Klein (KK) scale. Finally, I'll present exclusion plots which underline favourable values for the 6D gravity and KK scales, as a function of the mass of the brane particle whose loop breaks SUSY.

Time: 2 pm
Place: DRL 2N36

Rindler horizon perturbations and entanglement entropy
The Rindler horizon has thermal properties analogous to black hole horizons. Its classical area perturbations should therefore satisfy mechanical laws analogous to the classical laws of black hole mechanics. I will present a derivation of these laws in the context of perturbative general relativity, treated like a spin-2 field on flat spacetime in the tradition of Weinberg and Feynman. When the theory is quantized perturbatively, these can be promoted to laws of thermodynamics. The entropy of the horizon coincides with its Noether charge and, under certain circumstances, its dynamical changes can be identified exactly with changes in entanglement entropy.

Time: 2 pm
Place: DRL 2N36

Title: Electroweak exotics and dark matter from anomaly nucleation constraints
Place: DRL 2N36
Time: 2pm