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

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.

Investigating the Origin of the Long-Duration High- Energy Gamma-Ray Flares Gerry Share, Jim Ryan and Ron Murphy (in absentia) Steering Committee Overseer.

Particle acceleration in a turbulent electric field produced by 3D reconnection Marco Onofri University of Thessaloniki.

Energy Release and Particle Acceleration in Flares Siming Liu University of Glasgow 9 th RHESSI Workshop, Genova, Italy, Sep

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.

MHD modeling of coronal disturbances related to CME lift-off J. Pomoell 1, R. Vainio 1, S. Pohjolainen 2 1 Department of Physics, University of Helsinki.

“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.

Collisionless Magnetic Reconnection J. F. Drake University of Maryland Magnetic Reconnection Theory 2004 Newton Institute.

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.

Electron Acceleration at the Solar Flare Reconnection Outflow Shocks Gottfried Mann, Henry Aurass, and Alexander Warmuth Astrophysikalisches Institut Potsdam,

Institute of Astronomy, Radio Astronomy and Plasma Physics Group Eidgenössische Technische Hochschule Zürich Swiss Federal Institute of Technology, Zürich.

The Structure of the Parallel Electric Field and Particle Acceleration During Magnetic Reconnection J. F. Drake M.Swisdak M. Shay M. Hesse C. Cattell University.

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

SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps [session no.]1 I: C1/M8/C10 Transients: Drivers & Destabilization.

Theory of Shock Acceleration of Hot Ion Populations Marty Lee Durham, New Hampshire USA.

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

Joe Giacalone and Randy Jokipii University of Arizona

In-situ Observations of Collisionless Reconnection in the Magnetosphere Tai Phan (UC Berkeley) 1.Basic signatures of reconnection 2.Topics: a.Bursty (explosive)

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.

Kinetic Entry of Energetic Ions into the Magnetosphere A brief overview of a planned SolarCism contribution Dietmar Krauss-Varban Yan Li Janet Luhmann.

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.

F1B: Determine the Dominant Processes of Particle Acceleration Phase , Open the Frontier UV Spectroscopic determin- ation of pre/post-shock density,

Coronal and Heliospheric Modeling of the May 12, 1997 MURI Event MURI Project Review, NASA/GSFC, MD, August 5-6, 2003 Dusan Odstrcil University of Colorado/CIRES.

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

High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.

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

Cosmic Rays in the Heliosphere J. R. Jokipii University of Arizona I acknowledge helpful discussions with J. Kόta and J. GIacalone. Presented at the TeV.

Challenges in Understanding 3D Magnetic Reconnection in Observations and Simulations Session organizers: Peter Wyper (NASA Goddard Space Flight Center/Oak.

Hirotaka Ito Waseda University Collaborators Motoki Kino SISSA ISAS/JAXA ISS Science Project Office Naoki Isobe ISAS/JAXA ISS Science Project Office Nozomu.

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.

Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,

LOFAR & Particle Acceleration: Radio Galaxies & Galaxy Clusters

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

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

Collisionless Magnetic Reconnection J. F. Drake University of Maryland presented in honor of Professor Eric Priest September 8, 2003.

COSPAR 2004, Paris D July 21, 2004 THE HELIOSPHERIC DIFFUSION TENSOR John W. Bieber University of Delaware, Bartol Research Institute, Newark.

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,

Particle Transport in the Heliosphere: Part 1 Gaetano Zimbardo Universita’ della Calabria, Cosenza, Italy with contributions from S. Perri, P. Pommois,

Energy Budgets of Flare/CME Events John Raymond, J.-Y. Li, A. Ciaravella, G. Holman, J. Lin Jiong Qiu will discuss the Magnetic Field Fundamental, but.

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

Roles of Cosmic Rays in Galaxy Clusters Yutaka Fujita (Osaka U)

Cluster 911 Plasmoid Substorm Sept 11, 2002 DOY 254 Onset at 1600 UT Shock at Cluster 16:23 Plasmoid 16: :40 UT.

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

WG3 Session#3 Thursday PM: This session focused on the global effects of the Sun as seen in the outer heliosphere. The largest solar energetic particle.

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

Session 8: Particle Acceleration and Transport in Flares and their Relationship to SEP Events Antoun Daou David Alexander Rice University 2011 SHINE WORKSHOP.

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

Turbulence in the Solar Wind

Solar and heliosheric WG

Physics of Solar Flares

Session: Connecting Slow Wind Theories to Current and Future Observations by Justin Edmondson, Ben Lynch, Aleida Higginson, Xudong Sun and Liang Zhao.

NASA’s MMS Uncovers Dance of Electrons in Space

Field-Particle Correlation Experiments on DIII-D Frontiers Science Proposal Under weakly collisional conditions, collisionless interactions between electromagnetic.

T. Laitinen, S. Dalla Jeremiah Horrocks Institute, UCLan, UK

Introduction to Space Weather Interplanetary Transients

Particle Acceleration at Coronal Shocks: the Effect of Large-scale Streamer-like Magnetic Field Structures Fan Guo (Los Alamos National Lab), Xiangliang.

Fermi Collaboration Meeting

Student Day Working Group III summary

Steven R. Spangler University of Iowa

Acceleration of Electrons and Protons by Plasma Waves in Sgr A*

Diffusive Shock Acceleration

Heavy-Ion Acceleration and Self-Generated Waves in Coronal Shocks

Introduction to Space Weather

MHD Simulation of Plasmoid-Induced-Reconnection in Solar Flares

Proton Injection & Acceleration at Weak Quasi-parallel ICM shock

Presentation transcript:

Session 8: Global implications of kinetic-scale particle acceleration throughout the heliosphere Conveners: J. Dahlin, L. Wilson, B. Chen, J. Giacalone, K. Klein Science Questions What role does kinetic physics play in particle acceleration processes? F. Guo, H. Arnold agree: kinetic-scale dissipation not important in reconnection acceleration S. Du: Simulations of energization during island merger (reconnection), demonstrated energy gain term associated with agyrotropy E. Lichko: Magnetic pumping model generates proton v^-3 spectrum in less than an earth-to-sun transit time E. Lichko S. Du

Session 8: Global implications of kinetic-scale particle acceleration throughout the heliosphere Conveners: J. Dahlin, L. Wilson, B. Chen, J. Giacalone, K. Klein In what ways are turbulence, reconnection, and shock physics intertwined in the context of particle acceleration? S. Du: Observations of particle acceleration associated with flux ropes downstream of a weak shock observed by 5 AU & models (L. Zhao+ submitted) What observational signatures can be used to distinguish and constrain kinetic acceleration mechanisms? L. Wilson: Many injection/acceleration mechanisms at shocks, showed catalogue of distinct signatures associated with each A. Johlander: Survey of MMS bow shock crossings in burst mode: efficient ion energization for quasi-parallel, no correlation with mach number L. Zhao A. Johlander

Session 8: Global implications of kinetic-scale particle acceleration throughout the heliosphere Conveners: J. Dahlin, L. Wilson, B. Chen, J. Giacalone, K. Klein What additional observations and models are needed to make progress on the problem of particle acceleration? Kinetic simulations give insight on what physics is necessary to capture reconnection particle acceleration H. Arnold: new “hybrid” MHD model + guiding-center particles includes feedback from anisotropy F. Guo: MHD equation + Parker equation solution, acceleration via compression How strong is the turbulence? B. Chen: Type III bursts in VLA reveal large density variation in a small region – compression? B. Chen: radio emission from density perturbations at shock – turbulence? Can we observe/determine turbulence properties in reconnecting current sheet flares (e.g. scattering, energy content)? F. Guo B. Chen