PPT-The effect of turbulence upon supernova neutrinos

Jim Kneller NC State University NOW 2010 The neutrinos we will detect from the next SN in our Galaxy will tell us much about the explosion and the neutrino The flavour content of the signal changes as it propagates from the protoneutron star to our detectors here on Earth. No subscriber or other reader should act on the basis of any such information without referring to applicable laws and regulations andor without taking appropriate professional advice Although every effort has been made to ensure accuracy the Intern From . Dark Matter . Annihilation. Jason Kumar. University of. H. a. w. a. i. i. collaborators. Jin In. Carsten. . Rott. Pearl Sandick. Jennifer Gaskins. David Yaylali. 1502. 02091, 15xx.xxxxx. dark matter and monoenergetic neutrinos. http://turb.seas.ucla.edu/~jkim/sciam/turbulence.html Turbulence ? Why do the skin of sharks have groves ? Related Links But what exactly is turbulence? A few everyday examples may be illuminati Cecilia Lunardini. Arizona State University . And RIKEN BNL Research Center. INT workshop “Long-Baseline Neutrino Physics and Astrophysics”. Motivations . Current status. The future:. Detection potential. Rebecca . Bertsch. Advisor: Dr. . Sharath. . Girimaji. March 29, 2010. Supported . by: NASA MURI and Hypersonic Center. Outline . Introduction. RDT Linear Analysis of Compressible Turbulence. Method. Superfluid. . 4. He in the . T . = 0 Limit. Andrei . Golov. Paul . Walmsley. , Sasha . Levchenko. , Joe . Vinen. , Henry Hall, . Peter . Tompsett. , Dmitry . Zmeev. , . Fatemeh. . Pakpour. , Matt Fear. Physics Opportunities with. Supernova Neutrinos. Georg Raffelt, Max-Planck-Institut für Physik, München. Sanduleak -69 202. Sanduleak . -. 69 202. Large Magellanic Cloud . Distance 50 kpc . (160.000 light years). 1. John Beacom, The Ohio State University. 2. Plan of the Talk. Introduction to Supernova . N. eutrinos. Focus on . B. urst . D. etection. . What will we know after the next burst?. What . new capabilities do we need?. local winds. Scales of Atmospheric Motion vs. Lifespan. We’ve already started to investigate some of the synoptic-scale features…. Topics for today’s discussion. Basically here’s our roadmap for the rest of the course.. R.Svoboda. Sterile Neutrinos as DM?. As WIMP searches getting well below the weak interaction scale for large range of masses and collider limits now limit smaller masses. What if no . WIMPs. are found to well below weak scale?. Be . Majorana. States?. and Other Puzzlers Inspired by Adrian Melissinos. KT . McDonald. Princeton U. .. (March 7, 2017). Seminar at University . of Rochester. http://physics.princeton.edu/~. mcdonald/examples/majorana_170307.pptx. Neutrinos. Ghost . Particles . of the . Universe. Georg G. Raffelt. Max-Planck-Institut f. ür Physik, München, Germany. Neutron. Proton. Gravitation (Gravitons?) . Weak . Interaction (W and Z Bosons). with WFIRST . DRM1 and DRM2. C Baltay. June 1, 2012. Supernova Surveys . using . Slitless. Spectroscopy. Use Imager for . SNe. discovery and to get . lightcurves. Use . slitless. spectroscopy to type supernovae and get redshifts. ?. History in the Making?. 1862: Maxwell found that there should be electromagnetic waves travelling at approximately the (known) speed of light. 1905: Einstein used universal speed of light as foundation of geometric description of physics.