PPT-Roles of Cosmic Rays in Galaxy Clusters

Yutaka Fujita Osaka U Content CRs may be playing more important roles in clusters than you imagine Cosmic ray CR heating of cluster cores Fujita amp Ohira 2011 2012 2013 Fujita Kimura amp Ohira 2013. Noda and Y Kamide Supervised by Y Muraki brPage 2br Have you ever had an Xray examination at the hospital In 1896 a German physicist W C R57590ntgen astonished people with an image of bones captured through the use of Xrays He had just discovered th Douglas Bergman. University of Utah. Cosmic Rays – LHC Workshop, ECT* Trento. 2 December 2010. The Final Word (almost). HiRes Collaboration. J. Boyer, B. Connolly, C.B. Finley, B. Knapp, E.J. . Mannel. The Future of Cosmic Ray Research. .. 8 The Future of Cosmic Ray Research . As we have seen, a few cosmic rays can be detected with energies somewhat . greater . than 10. 20. . eV. . . These high energies must be due to particle accelerations . AMS Discoveries Affecting Cosmic-Ray SIG Priorities. Eun-Suk. . Seo. Inst. for Phys. Sci. & Tech. and . Department of Physics. University of Maryland. AAS HEAD meeting, Chicago, IL, 19 August 2014. Andrea . Chiavassa. Universita. ` . degli. . Studi. . di. Torino. Carpathian Summer School of Physics 2012. June 24 – July 7, . Sinaia. , Romania. Most of the material comes from the book:. “. the merger/. sloshing. . cold. front . paradigm. :. A2142 . revisited. by XMM. Mariachiara Rossetti. (Università degli Studi di Milano & IASF Milano). D. . . Eckert. , S. De Grandi, S. . Molendi. . Reionization. . . Chris . Carilli. (. M/N. RAO). Vatican Summer School June 2014. I. Introduction: Cosmic . Reionization. Concept . . Cool gas in z > 6 galaxies: quasar hosts. Constraints on evolution of neutral Intergalactic Medium (IGM). galaxy group, Stephan S. R. Kulkarni. Caltech Optical Observatories. Key Papers. “On Supernovae” Baade & . Zwicky. (1934a). “Cosmic Rays From Supernovae” Baade & . Zwicky. (1934b). “On the Search for Supernovae” . The Discovery of Antimatter!. In 1932 Carl Anderson studied cosmic rays using a “cloud . chamber”. . Charged particles produced in cosmic rays would enter the chamber and leave “tracks”. The tracks would bend in circles because the chamber was placed in a strong magnetic field. :. . the need for cross section data. Fiorenza Donato. Torino University and INFN. Compass Analysis Meeting. CERN, 16.04.2015. Plan of my talk. What are cosmic rays (CRs). Searches for dark matter in CRs. Plasma. . Astrophysics. Roger . Blandford. Paul Simeon. Yajie. Yuan. KIPAC. Stanford. 27 i 2012. AronsFest. 2. Describing Cosmic Plasma. Fluid description. P. , . . , . v. , B…. Magneto Fluid Dynamics . Eun-Suk. . Seo. Inst. for Phys. Sci. & Tech. and . Department of Physics. University of Maryland. AAS HEAD meeting, Chicago, IL, 19 August 2014. w. ith edits & voice from . Angela V. Olinto. 16 – 20 March 2015. Cosmic Rays: the current position -. from AMS to the Auger Observatory. 1. Alan Watson. University of Leeds. a.a.watson@leeds.ac.uk. Lecture 1:. Overview of the cosmic ray scene.