Weekly on Friday 11:30 am - 12:30 pm, in PRB M2005

COMING UP!

11:30 am, Friday, Feb 24th in PRB M2005 (Price Place) 


2017





11:30 am, Friday, Feb 3rd in PRB M2005 (Price Place) 
  1. Secondary Cosmic Positrons in an Inhomogeneous Diffusion Model
  2. for the 3.5 keV Line in the Deep Fields with Chandra: the 10 Ms observations
  3. Closing in on Resonantly Produced Sterile Neutrino Dark Matter
  4. First search for gravitational waves from known pulsars with Advanced LIGO
  5. Muon Beam Experiments to Probe the Dark Sector
  6. Probing Left-Right Seesaw using Beam Polarization at an e+e− Collider
  7. Unveiling ν secrets with cosmological data: neutrino masses and mass hierarchy
  8. Constraining Secluded Dark Matter models with the public data from the 79-string IceCube search for dark matter in the Sun
  9. 2013-2016 review: HE Neutrino and UHECR Astronomy?
  10. Ultrahigh energy cosmic ray nuclei from remnants of dead quasars

11:30 am, Friday, Jan 27th in PRB M2005 (Price Place) 

    Special Talk!
    
    Speaker: 
Oindree Banerjee (OSU)


11:30 am, Friday, Jan 20th in PRB M2005 (Price Place) 

    Special Talk!
    
    Speaker: 
Evan Grohs (U. of Michigan)

    Title: 
Big bang nucleosynthesis in neutrino cosmology

    
Abstract:
        
Cosmic microwave background Stage-IV experiments and thirty-meter-class telescopes will come online in the next decade.  The convolution of these data sets will provide on order 1% precision for observables related to neutrino cosmology.  Beyond Standard Model (BSM) physics could manifest itself in slight deviations from the standard predictions of quantities such as the neutrino energy density and the primordial abundances from Big Bang Nucleosynthesis (BBN).  In this talk, I will argue for the need for precise and accurate numerical calculations of BBN.  I will first show the detailed evolution of the neutrino spectra as they go out of equilibrium with the plasma.  The spectra are important in changing the ratio of neutrons to protons. I will show how sensitive the primordial mass fraction of helium is to the weak interaction rates which evolve the neutron-to-proton ratio.  Finally, I will present an example of how BSM physics can affect BBN by instituting an asymmetry between neutrinos and antineutrinos, commonly characterized by a lepton number.