PPT-Fast radio bursts and the magnetization and turbulence of t

w eb Ryan Shannon ICRARCurtin ATNF Vikram Ravi Swinburne Pulsar Group Outline Fast radio bursts FRBs Exciting times FRB 131104 The improbablerealtime discovery of an FRB to the Carina dwarf spheroidal. Nagesh brPage 2br RADIO CAB he radio taxi business is taking off in a big way in India with several private operators investing large sums in setting up call centres acquiring a 64258eet of new cars incorporating latest gadgets in their vehicles and Alexander . Kotov. , . ChengXiang. . Zhai. , Richard . Sproat. University of Illinois at Urbana-Champaign. Roadmap. Problem definition. Previous work. Approach. Experiments. Summary. Motivation. Web data is generated by a large number of textual streams (news, blogs, tweets, etc. Solar Energetic Particle Events . (L. . Winter, . S. Huston, K. . Ledbetter, R. Quinn; AER). Analysis of the Wind/WAVES radio burst and the GOES proton properties led to finding that radio properties (e.g., type II and type III peak flux) can be used to predict the peak proton flux level.. Poonam Chandra. National Centre for Radio Astrophysics - Tata Institute of Fundamental Research. Collaborator: Dale Frail and many others. Radio Afterglows. . Late time follow up.. . Accurate energetics instead of “isotropic equivalent” energy .. 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.. 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 T. Ostler. 1. Dept. . of Physics, The University of York, York, United Kingdom. .. December . 2013. Increasing demand. A few GB to TB’s. 25TB daily log. 100TB storage. 2.5PB. 24PB daily. 330 EB demand in 2011. Edwin Kite (U. Chicago), John Armstrong (Weber State), . Robin Wordsworth (Harvard), Francois Forget (LMD) . c. an climate . models. h. elp distinguish. these scenarios?. h. abitable surface. s. terile surface. Bas van de . Wiel. , . Ivo. van . Hooijdonk. & Judith . Donda. in collaboration with:. Fred . Bosveld. , Peter Baas, . Arnold . Moene. , Harm . Jonker. , . Jielun. Sun, Herman Clercx, . e.a. .. We thank Advanced Conductor Technologies and University of Colorado, Department of Physics, Boulder, CO, USA. D. van . der. . Laan. Center for Superconducting & Magnetic . Materials . (CSMM), The Ohio State University, Columbus, OH, USA. catch a burst and notify other observatoriesboth in space and on the ground of its approx-imate locationWithin minutes HETE-2 mayobtain a precise locationCurrent telescopestake much longer to notify o National Centre for Radio Astrophysics. Tata Institute of Fundamental Research. Poonam Chandra. What are Gamma Ray bursts (GRBs)?. Most energetic events in the universe. Long duration GRBs (t>2s) . S. Ku et al.. A fast edge turbulence bifurcation achieved in XGC1 when heat accumulation ~P. L-H. in the edge layer. in an L-mode diverted C-Mod edge geometry. with neutral particle recycling (R=0.99). High . ν. *. . Low. . ν. *. Empirical confinement scaling B. τ. E. .  . ν. *. -0.8. . in agreement with gyrokinetic GS2 simulations of ETG turbulence. BES measurements of ITG ñ show flow shear breaks symmetry of turbulence in space (tilt) and amplitude (skewed PDF).