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

COMING UP!

11:30 am
, Friday, Jun 23rd in PRB M2005 (Price Place)
  

    Special Talk!
    
    Speaker:  Linda Cremonesi (University College London)

    Title: The secrets of oscillating neutrinos at the NOvA experiment


    
Abstract:  

        Neutrino oscillations have first been observed almost 20 years ago, yet some fundamental parameters of the oscillation mechanism still need precise measurements. Do muon and tau neutrinos maximally mix? What is the neutrino mass ordering, normal or inverted? Is there CP violation in the lepton sector, and could this explain the matter/anti-matter asymmetry in the universe?

The NOvA experiment aims to answer these questions and much more. Muon neutrinos are produced at Fermilab in Illinois, and directed 810km towards Minnesota, where the disappearance of muon neutrinos and the appearance of electron neutrinos is measured. This talk will present the latest exciting results coming from the NOvA experiment!

  1. Evidence of internal dissipation origin for the high energy prompt emission of GRB~170214A
  2. First results from the NEWS-G direct dark matter search experiment at the LSM
  3. Probing decaying heavy dark matter with the 4-year IceCube HESE data
  4. The TUS detector of extreme energy cosmic rays on board the Lomonosov satellite
  5. Effects of self-generated turbulence on Galactic Cosmic Ray propagation and associated diffuse gamma-ray emission
  6. The Spatially Uniform Spectrum of the Fermi Bubbles: the Leptonic AGN Jet Scenario
  7. Universal cosmic rays energy spectrum and the mass composition at the 'ankle' and above
  8. Hydrogen Clouds from Comets 266P Christensen and P2008 Y2 (Gibbs) are Candidates for the Source of the 1977 WOW!Signal


2017

11:30 am, Friday, Jun 9th in PRB M2005 (Price Place)  
  1. High-energy cosmic ray nuclei from tidal disruption events: origin, survival, and implications
  2. First star formation in ultra-light particle dark matter cosmology
  3. Dark Matter Limits From Dwarf Spheroidal Galaxies with The HAWC Gamma-Ray Observatory
  4. High energy neutrinos from the Sun
  5. First all-flavour Neutrino Point-like Source Search with the ANTARES Neutrino Telescope
  6. Thermal Electrons in GRB Afterglows
  7. Is there anybody out there?
  8. A self-consistent model of cosmic-ray fluxes and positron excess: Roles of nearby pulsars and a sub-dominant source population
  9. Implications of supernova remnant origin model of galactic cosmic rays on Gamma rays from young supernova remnants
  10. Constraining high-energy neutrino emission from choked jets in stripped-envelope supernovae
  11. Supernovae in compact star clusters as sources of high-energy cosmic rays and neutrinos





11:30 am, Friday, May 19th in PRB M2005 (Price Place)  

    Special Talk!
    
    Speaker: 
Juri Smirnov (INFN)

    Title: 
Dark Matter Bound States

    
Abstract:
        
I will discuss the importance of bound state formation in processes relevant for dark matter physics. Such as the relic density computation and possible late time interactions leading to a indirect detection signature. It will be argued that bound state formation is a logical continuation of Sommerfeld enhancement and can even become the dominant non-relativistic effect in certain regimes. I will discuss spectra from WIMP dark matter capture processes allowing to obtain spectroscopic information on the structure of dark matter interactions.  The talk is based on the following recent work 1702.01141.



11:30 am, Friday, May 5th in PRB M2005 (Price Place)
  


11:30 am, Friday, Apr 21st in PRB M2005 (Price Place)
 


11:30 am, Friday, Apr 7th in PRB M2005 (Price Place)  

    Special Talk!
    
    Speaker: 
Nicholas Rodd (MIT)

    Title: 
Gamma-ray Constraints on Decaying Dark Matter and Implications for IceCube

    
Abstract:
        
Utilizing the Fermi measurement of the gamma-ray spectrum toward the inner Galaxy, I will explain how to derive some of the strongest constraints on dark matter lifetimes in the mass range from hundreds of MeV to above an EeV. The limits derived disfavour a decaying DM interpretation of the astrophysical neutrino flux observed by IceCube, and I will review why that possibility has received some attention in the literature recently.


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

11:30 am, Friday, Mar 10th in PRB M2005 (Price Place)
  


11:30 am, Friday, Mar 3rd in PRB M2005 (Price Place)  
  1. The Dark Side of MSW: Solar Neutrinos as a Probe of Dark Matter-Neutrino Interactions
  2. Offsets between member galaxies and dark matter in clusters: a test with the Illustris simulation
  3. Observations of M31 and M33 with the Fermi Large Area Telescope: a galactic center excess in Andromeda?
  4. Can BL Lac emission explain the neutrinos above 0.2 PeV?
  5. Constraints on the flux of ∼(10^16−10^17.5) eV cosmic photons from the EAS-MSU muon data
  6. Search for relativistic magnetic monopoles with five years of the ANTARES detector data
  7. Testing Lorentz invariance of dark matter with satellite galaxies
  8. HAWC Observations Strongly Favor Pulsar Interpretations of the Cosmic-Ray Positron Excess
  9. The nightmare scenario: measuring the stochastic gravitational-wave background from stalling massive black-hole binaries with pulsar-timing arrays
  10. Enabling Forbidden Dark Matter
  11. Why T2K should run in dominant neutrino mode to discover CP violation ?
  12. Collective neutrino oscillations and neutrino wave packets

11:30 am, Friday, Feb 24th in PRB M2005 (Price Place) 
  1. Electron train backgrounds in liquid xenon dark matter search detectors are indeed due to thermalization and trapping
  2. Nonmaximal θ23 mixing at NOvA from neutrino decoherence
  3. Extending the search for muon neutrinos coincident with gamma-ray bursts in IceCube data
  4. New constraints and discovery potential of sub-GeV dark matter with xenon detectors
  5. Distinguishing between Dirac and Majorana neutrinos in the presence of general interactions
  6. Scanning the Earth with solar neutrinos and DUNE
  7. Multiwavelength follow-up of a rare IceCube neutrino multiplet
  8. Search for right-handed neutrinos from dark matter annihilation with gamma-rays





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.