PPT-Acceleration of Solar Energetic Particles

Rami Vainio University of Helsinki Department of Physics Finland University of Turku Department of Physics and Astronomy Finland SPACECAST Stakeholder Meeting BAS 7 February 2014 Solar energetic particle events. mark the time of a shock passage by ACE and the dashed lines mark the onset of the 1 8 A X-ray flare (GOES). We acknowledge the use of data to the ACE, STEREO and GOES Science Teams. Such large SEP Mark . A. Clilverd. British . Antarctic Survey, Cambridge, United . Kingdom. With contributions from. Craig Rodger, University of . Otago. , Dunedin, New Zealand. Annika Seppälä, . Finnish Meteorological Institute, Helsinki, Finland. 1. Can we use the morphological matrix to answer the question ? . The « morphological box » of Fritz Zwicky. « everybody a genius ». 2. gravity. Acceleration. stars. particles. light. explosion. Exploring the Sun-. heliosphere. connection. Science questions. Mission overview. Status update. The Sun creates the heliosphere. Why study the Sun-space connection?. Addresses ESA’s Cosmic Vision question “How does the solar system work?”. Acceleration and . Transport Link of the Chain. J. . Giacalone. , University of Arizona. Mihir. Desai, . SWRI. Gang Li, University of Alabama. Nathan . Schwadron. , . UNH. (and others … ). “Sun to Ice” kick-off meeting – Predictive Science Inc., San Diego, Nov 2, 2011. Particles . Interaction . with the . Non-resonant Internal . Kink in Spherical . Tokamaks. Feng Wang*, G.Y. Fu**, J.A. Breslau**, E.D. Fredrickson**, J.Y. Liu*. *Dalian University of Technology, Dalian, China. (Fermi acceleration at shock: most standard, nice powerlaw, few free parameters). main . signatures to . be determined: . E. min . , . E. max. [. Ã. timescale . t. acc. (E. ) ], . spectral slope . Hadronic. Final State Reconstruction in Collider Experiments. (Part II). Peter Loch. University of Arizona. Tucson, Arizona. USA. Principles of . Calorimetry. Detector needs for multi-purpose collider experiments. Radiation Impacts on Space Weathering: . Mercury – Mars. . John . F. Cooper, . Heliospheric. Physics Laboratory, NASA . Goddard Space Flight Center. $8B Selfie! JWST and Me. Solar and . heliospheric. in a Developing Turbulence. . Shuichi M. ATSUKIYO. . ESST Kyushu Univ.. Collaborator : T. . Hada. Outline . Background. -- motivation. -- acceleration processes in turbulent plasmas. -- parametric instability (PI). THREE PHASES OF PARTICLE ACCELERATION. FLARE IMPULSIVE PHASE (. FIRST. ) FLARE LATE PHASE (. SECOND. ) . CME. SHOCK. IMPULSIVE SEP EVENT. GRADUAL SEP EVENT. FLARE. CME SHOCK. NOTE: NO Flare. NO/very little scattering except near shock. this can be e. −. , . . , protons, neutrons, excited nuclei, fragmented nuclei.... . . Spontaneous radiation and permanent activation is produced.. . Large variety of Beam Loss Monitors (. HSSIP-Project presentation: Elias . Kunze. & Julia . Nehlin. Electromagnetic interactions:. E. lectron-positron scattering . E. lectron-electron scattering . P. hoton-electron scattering . P. hoton . 1. NIFS . NINS, . 2. SOKENDAI, . 3. Kyushu . Univ. ., . 4. ORNL. 16th Technical Meeting on Energetic Particles in Magnetic Confinement Systems – Theory of Plasma Instabilities. K. Ogawa. 1,2. , M. Isobe.