PPT-Supernova Burst and Relic Neutrinos

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. Neutrino . L. imits. Georg G. Raffelt, Max-Planck-Institut f. ür Physik, München. Sun. Globular Cluster. Supernova 1987A. Cosmology. Questions about Neutrinos. Standard properties of active 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 proto-neutron star to our detectors here on Earth.. :. past present future. Heidi Schellman @ Frank Merritt Fest 2015. 1. What we knew in 1971. 2. Neutrinos exist (Cowan, . Reines. 1956). There are two kinds (Lederman, Schwartz, Steinberger - 1962 ). 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. R.Svoboda. November 23, SLAC. 1. DUNE. 2. 3. Steel Cryostat. 12 m. 14.4 m. 3.6m. DUNE Far Detector Conceptual Design. Detector Parameters (One 10-kton Module) . 58 m x 12 m x 14.4 m (~50 times larger than ICARUS. 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). 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. :. past present future. Heidi Schellman @ Frank Merritt Fest 2015. 1. What we knew in 1971. 2. Neutrinos exist (Cowan, . Reines. 1956). There are two kinds (Lederman, Schwartz, Steinberger - 1962 ). Instrument Chemistries for each step in the decontamination process. Pre-cleaning. Manual cleaning. Automated cleaning. Case Solutions. CSR Ink and adhesive remover. SchmutzOff stainless steel, acid based re-conditioner and . Instrument Chemistries for each step in the decontamination process. Pre-cleaning. Manual cleaning. Automated cleaning. © 2010 Case Medical, Inc.. Case Solutions. CSR Ink and adhesive remover. SchmutzOff stainless steel, acid based re-conditioner and . Most stars either have M < 1.4 . M. ʘ. , . or can lose enough mass during post-main sequence evolution to get there, and end as white dwarf. However if core is more massive, nothing can stop gravitational collapse. Shirley Li. The Ohio State University. Collaborators: Luke Roberts, John Beacom. TeVPA. , August 2017. Timescale of a SN. Shirley. . Li. (OSU). Figure. . credit. : . R.J. . Hall. ?. Detectable!. . Li, . Shuo. Supervisor: Prof. Moshe Zukerman. Co-supervisor: Dr. Eric W. M. Wong. Further Credits: Dr. V. . Abramov. , Dr. . Meiqian. Wang and Zhang . Jianan. Jan. 06, 2014. 1. Outline. Background: Optical burst switching (OBS). ?. 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.