Particle Acceleration by Relativistic Expansion of Magnetic Arcades

Slides:

Advertisements

Similar presentations

Physics of fusion power

Advertisements

Erdem Oz* USC E-164X,E167 Collaboration Plasma Dark Current in Self-Ionized Plasma Wake Field Accelerators

AS 4002 Star Formation & Plasma Astrophysics BACKGROUND: Maxwell’s Equations (mks) H (the magnetic field) and D (the electric displacement) to eliminate.

Magnetic dissipation in Poynting dominated outflows Yuri Lyubarsky Ben-Gurion University.

Relativistic Reconnection in Pairs: Mass Transport (Acceleration?) J. Arons UC Berkeley Question: How Does Return Current in PSR Magnetosphere Form? What.

Non-Equilibrium Ionization Modeling of the Current Sheet in a Simulated Solar Eruption Chengcai Shen Co-authors: K. K. Reeves, J. C. Raymond, N. A. Murphy,

Physics of fusion power Lecture 6: Conserved quantities / Mirror device / tokamak.

Relativistic Particle Acceleration in a Developing Turbulence Relativistic Particle Acceleration in a Developing Turbulence Shuichi M ATSUKIYO ESST Kyushu.

Physics 777 Plasma Physics and Magnetohydrodynamics (MHD) Instructor: Gregory Fleishman Lecture 12. Particle Acceleration 18 November 2008.

ASYMMETRIC THIN CURRENT SHEETS: A 1-D TEST PARTICLE MODEL AND COMPARISON WITH SW DATA J. Chen 1 and R. A. Santoro 2 1 Plasma Physics Division, Naval Research.

Physics of fusion power Lecture 8: Conserved quantities / mirror / tokamak.

Pei-Chun Hsu¹, Kouichi Hirotani², and Hsiang-Kuang Chang¹ 1 Department of Physics and Institute of Astronomy, National Tsing Hua University ASIAA/National.

Maser emission from relativistic shocks and electron-ion energy equilibration Yuri Lyubarsky Ben-Gurion University, Israel.

Center for Space Environment Modeling Ward Manchester University of Michigan Yuhong Fan High Altitude Observatory SHINE July.

UVCS Observations of the Solar Wind and its Modeling 6th Solar-B Science Meeting Kyoto, Japan, November 8–11, 2005 CMEs Coronal mass ejections (CMEs) are.

Solar system science using X-Rays Magnetosheath dynamics Shock – shock interactions Auroral X-ray emissions Solar X-rays Comets Other planets Not discussed.

Seed Population for Particle Acceleration... Anywhere in the Universe Shock heating based on many factors: v shock : shock speed  Bn : magnetic.

Collisionless shocks in Gamma Ray Bursts Current results and future perspectives. Århus, September 2005 Troels Haugbølle Dark Cosmology.

Magnetic Reconnection Rate and Energy Release Rate Jeongwoo Lee 2008 April 1 NJIT/CSTR Seminar Day.

Computationally efficient description of relativistic electron beam transport in dense plasma Oleg Polomarov*, Adam Sefkov**, Igor Kaganovich** and Gennady.

Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland

Cosmic Magnetic Fields: Helicity Injection by Supermassive Black Holes, Galaxies and Laboratory Experiments Hui Li 李暉 Los Alamos National Laboratory and.

Simulation of relativistic shocks and associated radiation from turbulent magnetic fields 2010 Fermi Symposium 9 – 12 May 2011 Rome Italy K.-I. Nishikawa.

Reconnection rates in Hall MHD and Collisionless plasmas

Valentina Zharkova 1 and Olga Khabarova Department of Mathematics, University of Bradford, Bradford BD7 1DP, UK ( ) 2.

PIC simulations of magnetic reconnection. Cerutti et al D PIC simulations of relativistic pair plasma reconnection (Zeltron code) Includes – Radiation.

Electron behaviour in three-dimensional collisionless magnetic reconnection A. Perona 1, D. Borgogno 2, D. Grasso 2,3 1 CFSA, Department of Physics, University.

3D Crab Model and comparison with Chandra result Pulsar Wind Nebulae and Particle Acceleration in the Pulsar Magnetosphere Shibata, S., Tomatsuri, H.,

Response of the Magnetosphere and Ionosphere to Solar Wind Dynamic Pressure Pulse KYUNG SUN PARK 1, TATSUKI OGINO 2, and DAE-YOUNG LEE 3 1 School of Space.

Kinetic MHD Simulation in Tokamaks H. Naitou, J.-N. Leboeuf †, H. Nagahara, T. Kobayashi, M. Yagi ‡, T. Matsumoto*, S. Tokuda* Joint Meeting of US-Japan.

Radiation spectra from relativistic electrons moving in turbulent magnetic fields ＹｕｔｏＴｅｒａｋｉ & Fumio Takahara Theoretical Astrophysics Group Osaka Univ.,

Simulation Study of Magnetic Reconnection in the Magnetotail and Solar Corona Zhi-Wei Ma Zhejiang University & Institute of Plasma Physics Beijing,

1-3 November nd EAST-ASIA NUMERICAL ASTROPHYSICS MEETING (KASI, Daejeon, Korea) Numerical Simulations of Relativistic Expansion of Magnetic Arcades.

The Structure of the Pulsar Magnetosphere via Particle Simulation S. Shibata (1), T. Wada (2), S. Yuki (3), and M. Umizaki (3) (1)Department of Phys.Yamagata.

Particle Acceleration by Relativistic Collisionless Shocks in Electron-Positron Plasmas Graduate school of science, Osaka University Kentaro Nagata.

Ehud Nakar California Institute of Technology Unmagentized relativistic collisionless shock Milos Milosavljevic (Caltech) Anatoly Spitkovsky (KIPAC) Venice.

XRT and EIS Observations of Reconnection associated Phenomena D. Shiota, H. Isobe, D. H. Brooks, P. F. Chen, and K. Shibata

AGN: Linear and Circular Polarization

November 1 - 3, nd East Asia Numerical Astrophysics Meeting KASI, Korea Shock Waves and Cosmic Rays in the Large Scale Structure of the Universe.

Gamma-Ray Bursts and unmagnetized relativistic collisionless shocks Ehud Nakar Caltech.

1 Magnetic components existing in geodesic acoustic modes Deng Zhou Institute of Plasma Physics, Chinese Academy of Sciences.

1 Joachim Birn LANL Karl Schindler Ruhr-Univ. Bochum Michael Hesse NASA/GSFC Thin Electron Current Sheets and Auroral Arcs Relationship between magnetospheric.

Stuart D. BaleFIELDS SOC CDR – Science Requirements Solar Probe Plus FIELDS SOC CDR Science and Instrument Overview Science Requirements Stuart D. Bale.

Electron-Scale Dissipations During Magnetic Reconnection The 17th Cluster Workshop May 12-15, 2009 at Uppsala, Sweden Hantao Ji Contributors: W. Daughton*,

Rapid high-energy emission variability in relativistic pair plasma reconnection Benoît Cerutti University of Colorado, USA. 5 th International Symposium.

Simulation of relativistic shocks and associated radiation from turbulent magnetic fields 2009 Fermi Symposium 2-5 November 2009 Hyatt Regency Washington,

Laser wake field acceleration using nano-particles Laser wake field acceleration using nano-particles Department of Physics and Photon Science, Gwangju.

Axel Brandenburg & Jörn Warnecke NorditaStockholm  loop emergence –Buoyant rise –Many scale heights –Twist needed Dynamo –bi-helical field Emergence.

Evolution of the poloidal Alfven waves in 3D dipole geometry Jiwon Choi and Dong-Hun Lee School of Space Research, Kyung Hee University 5 th East-Asia.

“Harris” Equilibrium: Initial State for a Broad Class of

Using a combined PIC-MHD code to simulate particle acceleration

Christina Chu University of Alaska Fairbanks Geophysical Institute

Tomoyuki Johzaki*, *Hiroshima University Energy density (Bx2+By2)1/2

Kinetic Structure of the Reconnection Layer and of Slow Mode Shocks

PIC code simulations of solar flare processes Astronomical Institute

An overview of turbulent transport in tokamaks

Simulation of laser ion-acceleration and transport

Olga Khabarova 1, valentina zharkova 2 & vladimir kuznetsov 1

The Magnetosphere Feifei Jiang, UCLA

Computational Methods for Kinetic Processes in Plasma Physics

The structure of the pulsar magnetosphere via particle simulation

Force acting on a charged particle moving through a magnetic field

Induction Equation Diffusion term Advection term

The Physics of the Collisionless Diffusion Region

Arianna Ligorini Department of Gamma-ray Astrophysics Institute of Nuclear Physics PAS, Krakow Jacek Niemiec Department of Gamma-ray Astrophysics Institute.

Intense Coherent Emission in Relativistic Shocks

MHD Simulation of Plasmoid-Induced-Reconnection in Solar Flares

The Motion of Charged Particles in Magnetic Fields

V. Rozhansky1, E. Kaveeva1, I. Veselova1, S. Voskoboynikov1, D

Chapter 28 Magnetic Fields

Presentation transcript:

Particle Acceleration by Relativistic Expansion of Magnetic Arcades H. Takahashi, E. Asano, R. Matsumoto Chiba Unv. Japan shock current sheet Asano et al. (P12)

Simulation Model of Particle Accelerations 2-dim. Paritcle-In-Cell (PIC) simulation Mikic Model extended into relativistic plasma (NX,NY)=(200,1600) Assumption elecron-positron plasma collisionless Plasma density is slightly larger than Goldreich-Julian density Initial Model constructed by Mikic(‘88) Bz : toroidal components Bx,By: poloidal components

2.5-dimensional PIC Simulation: Result Tg=90.0 Tg=237.5 color: Bz line: field line color: density line: field line color: Bz line: field line ExB drift motion leads to charge deficiency in the arcades. Magnetic reconnections take place inside the expanding arcades.