Shocks! David Burgess Astronomy Unit Queen Mary, University of London.

Slides:

Advertisements

Similar presentations

Experimental tasks Spectra Extend to small scale; wavenumber dependence (Taylor hyp.); density, flow Verify existence of inertial range Determine if decorrelation.

Advertisements

Progress and Plans on Magnetic Reconnection for CMSO For NSF Site-Visit for CMSO May1-2, Experimental progress [M. Yamada] -Findings on two-fluid.

Magnetic Turbulence in MRX (for discussions on a possible cross-cutting theme to relate turbulence, reconnection, and particle heating) PFC Planning Meeting.

Session A Wrap Up. He Abundance J. Kasper Helium abundance variation over the solar cycle, latitude and with solar wind speed Slow solar wind appears.

混合模拟基本方程与无量纲化基本方程. 无量纲化方程化为一些基本关系式 Bow shock and magnetosheath.

MHD Shocks and Collisionless Shocks Manfred Scholer Max-Planck-Institut für extraterrestrische Physik Garching, Germany The Solar/Space MHD International.

Study of shock non-stationarity with 1-D and 2-D hybrid simulations Xingqiu Yuan, Iver Cairns, School of Physics, University of Sydney, NSW, Australia.

“Physics at the End of the Galactic Cosmic-Ray Spectrum” Aspen, CO 4/28/05 Diffusive Shock Acceleration of High-Energy Cosmic Rays The origin of the very-highest-energy.

Alfvén-cyclotron wave mode structure: linear and nonlinear behavior J. A. Araneda 1, H. Astudillo 1, and E. Marsch 2 1 Departamento de Física, Universidad.

Quasilinear Analysis on Electron Heating in a Foot of a High Mach Number Shock Shuichi M ATSUKIYO ESST Kyushu University (

Modeling Generation and Nonlinear Evolution of VLF Waves for Space Applications W.A. Scales Center of Space Science and Engineering Research Virginia Tech.

Modeling Generation and Nonlinear Evolution of Plasma Turbulence for Radiation Belt Remediation Center for Space Science & Engineering Research Virginia.

Electromagnetic instabilities and Fermi acceleration at ultra-relativistic shock waves Electromagnetic instabilities and Fermi acceleration at ultra-relativistic.

Shock Source Description: Large-Scale Hybrid Simulations Dietmar Krauss-Varban Janet Luhmann Ilan Roth Yan Li Steve Ledvina Space Sciences Laboratory,

Solar Flare Particle Heating via low-beta Reconnection Dietmar Krauss-Varban & Brian T. Welsch Space Sciences Laboratory UC Berkeley Reconnection Workshop.

Computational Modeling Capabilities for Neutral Gas Injection Wayne Scales and Joseph Wang Virginia Tech Center for Space Science and Engineering.

Joe Giacalone and Randy Jokipii University of Arizona

Buneman and Ion Two-Stream Instabilities in the Foot Region of Collisionless Shocks Fumio Takahara with Yutaka Ohira (Osaka University) Oct. 6, 2008 at.

Hybrid simulations of parallel and oblique electromagnetic alpha/proton instabilities in the solar wind Q. M. Lu School of Earth and Space Science, Univ.

Particle Acceleration by MHD turbulence in Solar flares Huirong Yan (CITA) Collaborator: Alex Lazarian (UW-Madison)

Shock Wave Related Plasma Processes

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

GTC Status: Physics Capabilities & Recent Applications Y. Xiao for GTC team UC Irvine.

A Fermi Model for the Production of Energetic Electrons during Magnetic Reconnection J. F. Drake H. Che M. Swisdak M. A. Shay University of Maryland NRL.

Incorporating Kinetic Effects into Global Models of the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

The Injection Problem in Shock Acceleration The origin of the high-energy cosmic rays remains one of the most-important unsolved problems in astrophysics.

Monte Carlo simulations of the first-order Fermi process Niemiec & Ostrowski (2004) ApJ 610, 851 Niemiec & Ostrowski (2006) ApJ 641, 984 Niemiec, Ostrowski.

CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM SESSION 1B Discussion of.

Ion dynamics and shock front nonstationarity in supercritical perpendicular shocks: impact of the pickup ions Zhongwei YANG 1 and Quanming LU 2 1 SOA Key.

Modelling of the Effects of Return Current in Flares Michal Varady 1,2 1 Astronomical Institute of the Academy of Sciences of the Czech Republic 2 J.E.

Interaction among cosmic Rays, waves and large scale turbulence Interaction among cosmic Rays, waves and large scale turbulence Huirong Yan Kavli Institute.

Multiscale issues in modeling magnetic reconnection J. F. Drake University of Maryland IPAM Meeting on Multiscale Problems in Fusion Plasmas January 10,

Outstanding Issues Gordon Holman & The SPD Summer School Faculty and Students.

Diffusive shock acceleration: an introduction

Reconnection rates in Hall MHD and Collisionless plasmas

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

ESS 200C, Lecture 8 The Bow Shock and Magnetosheath Reading: Ch 5, 6 Kivelson & Russell.

Dispersive Waves and Magnetic Reconnection Alex Flanagan (University of Wisconsin) J. F. Drake (UMD), M. Swisdak (UMD)

IMPRS Lindau, Space weather and plasma simulation Jörg Büchner, MPAe Lindau Collaborators: B. Nikutowski and I.Silin, Lindau A. Otto, Fairbanks.

ALFVEN WAVE ENERGY TRANSPORT IN SOLAR FLARES Lyndsay Fletcher University of Glasgow, UK. RAS Discussion Meeting, 8 Jan

Ion pickup and acceration in magnetic reconnection exhausts J. F. Drake University of Maryland M. Swisdak University of Maryland T. Phan UC Berkeley E.

Electron Acceleration in Perpendicular Collisionless shocks with preexisting magnetic field fluctuations Fan Guo and Joe Giacalone With thanks to Dr. Randy.

SHINE 2006 Student Day Working Group III summary Zermatt, Utah, July 31 - August 4 Gang Li.

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

Non-thermal emission and particle acceleration by reverse shock in SNR ejecta Jiangtao Li

A new mechanism for heating the solar corona Gaetano Zimbardo Universita’ della Calabria Rende, Italy SAIt, Pisa, 6 maggio 2009.

Collisionless Shocks Manfred Scholer

MHD and Kinetics Workshop February 2008 Magnetic reconnection in solar theory: MHD vs Kinetics Philippa Browning, Jodrell Bank Centre for Astrophysics,

A shock is a discontinuity separating two different regimes in a continuous media. –Shocks form when velocities exceed the signal speed in the medium.

Solar Energetic Particles (SEP’s) J. R. Jokipii LPL, University of Arizona Lecture 2.

ISSI meeting 31 Mars-04 April Critical questions and tasks.

18 Nov 2010 Waves + Reconnection=? U of Warwick Astronomy Unit, School of Mathematical Sciences Vlasov-Maxwell and PIC,

Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetic Structure Feb. 16, 2012.

Solar energetic particle simulations in SEPServer How to deal with scale separation of thirteen orders of magnitude R. Vainio, A. Afanasiev, J. Pomoell.

A Global Hybrid Simulation Study of the Solar Wind Interaction with the Moon David Schriver ESS 265 – June 2, 2005.

Page 1 Collisionless and relativistic plasma astrophysics 2007 CRPA The quest for questions: a reflective summary of the discussion Monday: edited during.

Diffusive shock acceleration: an introduction

Kinetic Structure of the Reconnection Layer and of Slow Mode Shocks

The Magnetopause Back in 1930 Chapman and Ferraro foresaw that a planetary magnetic field could provide an effective obstacle to the solar-wind plasma.

ESS 154/200C Lecture 11 Collisionless Shocks

Dmitri Uzdensky (University of Colorado Boulder)

ESS 154/200C Lecture 19 Waves in Plasmas 2

Edison Liang, Koichi Noguchi Orestes Hastings, Rice University

The Bow Shock and Magnetosheath

In situ particle detection

Diffusive shock acceleration: an introduction – cont.

Diffusive Shock Acceleration

Session 8: Global implications of kinetic-scale particle acceleration throughout the heliosphere Conveners: J. Dahlin, L. Wilson, B. Chen, J. Giacalone,

Intense Coherent Emission in Relativistic Shocks

Proton Injection & Acceleration at Weak Quasi-parallel ICM shock

Presentation transcript:

Shocks! David Burgess Astronomy Unit Queen Mary, University of London

This presentation was given at: Workshop on Solar Kinetics and MHD, Feb 2008, RAL Cosener's House, Abingdon, UK. This is not a comprehensive tutorial about collisionless shocks in the solar context. The aim is only to give an indication of some current areas of interest in shock research, and in particular to draw attention to some areas and questions that could be interesting to pursue further in the context of the solar atmosphere and corona.

Shocks:  All the important physics is kinetic  Particle reflection  Instabilities  Particle acceleration Without collisions … Converting flow to thermal energy

What parameters are important? Shock normal angle : quasi-parallel versus quasi-perpendicular Mach Number Plasma beta Simulation method (hybrid, PIC, etc) Mass ratio Dimensionality

Some Topics … Electron acceleration Nonstationarity Turbulence

Electron Acceleration at Qperp Fast Fermi by mirror reflection Highest energies (but lowest efficiency) at close to perpendicular

Effect of including structure Test particle electrons in fields from 2D hybrid simulation Structure: power law energy spectra up and downstream

Nonstationarity at Qperp Shocks Hybrid: nonstationary at low enough  PIC: overturning via over-reflection of ions Effect controlled by  and mass ratio used in simulations …

Nonstationarity at Qperp Shocks With realistic mass ratio foot dynamics controlled by electromagnetic two stream instability With implications for (eg) shock surfing acceleration

Nonstationarity at Oblique Shocks PIC simulations Away from perpendicular, standing whistler can dominate structure Nonstationarity via competition of different mechanisms

Kinetic Effects in Turbulence Kinetics and the “dissipation” scale What is the “energy cascade” at kinetic scales? What happens with multiple kinetic scales? Control of temperature and temperature anisotropy with linear instabilities

Shocks in the Corona Flares …

Solar shocks continued … CME

More solar shocks?

Dynamic Fibrils - Simulations