Phenomenology 2014 Symposium

Session

Cosmology II

5 May 2014, 16:30

University of Pittsburgh

Conveners

Cosmology II

• Jay Hubisz (Syracuse University)

149. Cosmological Phase Transitions and their Properties in the NMSSM

Jonathan Kozaczuk (TRIUMF)

05/05/2014, 16:30

In this talk, I will discuss cosmological phase transitions in the Next-to-Minimal Supersymmetric Standard Model (NMSSM) in light of the Higgs discovery. I will focus on regions of the NMSSM with a viable neutralino dark matter candidate, > 1 TeV stops, and a Higgs sector compatible with current LHC results. I will show that the phase structure in the viable regions of parameter space can...

45. Generating the Observed Baryon Asymmetry from the Inflaton Field

Mark Hertzberg (MIT)

05/05/2014, 16:45

We propose a mechanism by which the inflaton can generate baryogenesis, by taking the inflaton to be a complex scalar field with a weakly broken global symmetry and present a new version of the Affleck-Dine mechanism. The smallness of the breaking is motivated both by technical naturalness and a requirement for inflation. We study inflation driven by a quadratic potential for simplicity and...

31. The Electroweak Vacuum Angle

Dr Hiren Patel (Max Planck Institute fur Kernphysik)

05/05/2014, 17:00

I describe the electroweak vacuum angle (the SU(2) analog of the QCD vacuum angle), and discuss conditions under which it becomes a physical parameter. I explain how its CP-violating effect enters into low and high energy observables, and I highlight its potentially important role in baryogenesis. Talk based on arXiv:1402.6340 and ongoing work.

33. Implementing MaVaNs Cosmology

Akshay Ghalsasi (University of Washington)

05/05/2014, 17:15

It has been shown that mass varying neutrinos (MaVaNs) can act as a negative pressure and hence are a candidate for dark energy.However MaVaNs also allow for higher $\Sigma$m$_\nu$ than terrestrial bounds, giving late forming warm dark matter. In this paper we implement MaVaNs cosmology using CMBEASY to study the effect of MaVaNs cosmology on the CMB spectrum. The MaVaNs parameter space...

1. On a singular solution in Higgs field (7) – The stiffness of candidate for dark energy, and the matter-antimatter consumption by candidate for dark matter

Kazuyoshi Kitazawa (Risp Japan)

05/05/2014, 17:30

Recently we discussed the degenerates into the candidates for dark matter (DM) and for dark energy (DE) from ur-Higgs boson 1, and also a long time behavior of DE 2. In this talk we at first study the stiffness of DE, by which the disruption interval of DE (i.e., expansion interval of the universe) would be determined. After calculating a critical collision number by considering the saturated...

36. Dark Matter Thermalization in Neutron Stars

Bridget Bertoni (U)

05/05/2014, 17:45

There have been many experimental efforts to constrain the dark matter - nucleon cross section as a function of dark matter mass. By considering black hole formation in neutron stars due to dark matter accretion, one can constrain dark matter parameter space that is inaccessible to current direct detection experiments. We have studied how Pauli blocking, kinematic constraints, and...

137. Constraining Hidden Sectors with Light from Cosmic Strings

Andrew Long (A)

05/05/2014, 18:00

A compelling minimal extension of the Standard Model consists of a TeV scale hidden sector that, from a phenomenological perspective, arises in dark matter model building and to motivate Z’ searches. If the hidden sector contains a spontaneously broken Abelian gauge symmetry, then our universe is permeated by a network of cosmic “dark strings.” These strings are far too light to be exposed...

101. Icezones vs. Firewalls

Dejan Stojkovic (SUNY at Buffalo)

05/05/2014, 18:15

We critically examine the assumptions made in the setup of the firewalls paradox. We point out several flaws which indicate that the paradox itself is not formulated in a self-consistent way. In particular, during the black hole evaporation, a mode of the late radiation is never simultaneously entangled with early radiation and a mode inside the horizon. We then go a step forward, and show...