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.
AstroParticle Lunch: "Big bang nucleosynthesis in neutrino cosmology" Evan Grohs (U. of Michigan)
January 20, 2017
11:30AM - 12:30PM
PRB M2005
Add to Calendar
2017-01-20 12:30:00
2017-01-20 13:30:00
AstroParticle Lunch: "Big bang nucleosynthesis in neutrino cosmology" Evan Grohs (U. of Michigan)
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.
PRB M2005
OSU ASC Drupal 8
ascwebservices@osu.edu
America/New_York
public
Date Range
Add to Calendar
2017-01-20 11:30:00
2017-01-20 12:30:00
AstroParticle Lunch: "Big bang nucleosynthesis in neutrino cosmology" Evan Grohs (U. of Michigan)
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.
PRB M2005
Center for Cosmology and AstroParticle Physics (CCAPP)
ccapp@osu.edu
America/New_York
public