Taiyou Zasshikai on May 17, 2004

Slides:

Advertisements

Similar presentations

Reames, Ng, Tylka 2012 Sol Phys Multi-spacecraft observation.

Advertisements

The magnetic nature of solar flares Paper by E.R. Priest & T.G. Forbes Review presented by Hui Song.

CME/Flare Mechanisms Solar “minimum” event this January For use to VSE must be able to predict CME/flare Spiro K. Antiochos Naval Research Laboratory.

Episodic magnetic jets as the central engine of GRBs Feng Yuan With: Bing Zhang.

Reviewing the Summer School Solar Labs Nicholas Gross.

Solar Energetic Particles and Shocks. What are Solar Energetic Particles? Electrons, protons, and heavier ions Energies – Generally KeV – MeV – Much less.

1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.

STEREO AND SPACE WEATHER Variable conditions in space that can have adverse effects on human life and society Space Weather: Variable conditions in space.

TOWARDS A REALISTIC, DATA-DRIVEN THERMODYNAMIC MHD MODEL OF THE GLOBAL SOLAR CORONA Cooper Downs, Ilia I. Roussev, Bart van der Holst, Noe Lugaz, Igor.

Center for Space Environment Modeling Numerical Model of Solar Eruption on 1998 May 2 Ilia Roussev, Igor Sokolov, & Tamas Gombosi.

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

Solar Energetic Particle Production (SEPP) Mission Primary Contacts: Robert P. Lin (UC Berkeley), John L. Kohl (Harvard-Smithsonian CfA) Primary Science.

Two energy release processes for CMEs: MHD catastrophe and magnetic reconnection Yao CHEN Department of Space Science and Applied Physics Shandong University.

The Sources of Solar Hazards in Interplanetary Space Leonard Strachan & Jun Lin (Harvard – Smithsonian Center for Astrophysics) Paper [72.05] “Contributions.

Center for Space Environment Modeling Numerical Model of Solar Eruption on 1998 May 2 Ilia Roussev, Igor Sokolov & Tamas Gombosi.

HMI/AIA Science Team Meeting, HMI Science Goals Alexander Kosovichev & HMI Team.

Center for Space Environment Modeling T. H. Zurbuchen, on behalf of W. Manchester, J. Kota, I. Roussev, T. H. Zurbuchen, N.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.

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

C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.

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.

Ward Manchester University of Michigan Coupling of the Coronal and Subphotospheric Magnetic Field in Active Regions by Shear Flows Driven by The Lorentz.

Generation of Solar Energetic Particles (SEP) During May 2, 1998 Eruptive Event Igor V. Sokolov, Ilia I. Roussev, Tamas I. Gombosi (University of Michigan)

Center for Space Environment Modeling Numerical Model of CME Initiation and Shock Development for the 1998 May 2 Event Ilia.

Space Weather Forecast With HMI Magnetograms: Proposed data products Yang Liu, J. T. Hoeksema, and HMI Team.

Center for Space Environment Modeling W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March.

C. May 12, 1997 Interplanetary Event. May 12, 1997 Interplanetary Coronal Mass Ejection Event CU/CIRES, NOAA/SEC, SAIC, Stanford Tatranska Lomnica, Slovakia,

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.

Elmau III, March 16, 2004 Coronal mass ejections A critical view of interpretations H.S. Hudson (UC Berkeley)

Modeling suprathermal proton acceleration by an ICME within 0.5 AU: the May 13, 2005 event K. A. Kozarev 1,5 R. M. Evans 2, M. A. Dayeh.

Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.

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

CME Initiation: The Matrix Reloaded David Alexander, Rice University.

Semi-Empirical MHD Modeling of the Solar Wind Igor V. Sokolov, Ofer Cohen, Tamas I. Gombosi CSEM, University of Michigan Ilia I Roussev, Institute for.

Abstract Although Parker was the first to describe the solar wind successfully at the time, his elegant theory still masks a number of fundamental problems.

1Yang Liu/Magnetic FieldHMI Science – 1 May 2003 Magnetic Field Goals – magnetic field & eruptive events Yang Liu Stanford University.

R. Oran csem.engin.umich.edu SHINE 09 May 2005 Campaign Event: Introducing Turbulence Rona Oran Igor V. Sokolov Richard Frazin Ward Manchester Tamas I.

1 THE RELATION BETWEEN CORONAL EIT WAVE AND MAGNETIC CONFIGURATION Speakers: Xin Chen

Three-dimensional MHD simulation of a flux rope driven CME Manchester IV, W.B., Gombosi, T.I., Roussev, I., De Zeeuw, D.L., Sokolov, I.V., Powell, K.G.,

The SEP Acceleration and Transport Link of the Chain

1 Introduction: Onset of solar flares and coronal mass ejections Yokoyama, T. Dept. Earth & Planetary Science, University of Tokyo Isobe, H. Univ. Tokyo.

1 SPD Meeting, July 8, 2013 Coronal Mass Ejection Plasma Heating by Alfvén Wave Dissipation Rebekah M. Evans 1,2, Merav Opher 3, and Bart van der Holst.

End-to-End Overview of Hazardous Radiation Len Fisk University of Michigan.

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.

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

A Numerical Study of the Breakout Model for Coronal Mass Ejection Initiation P. MacNeice, S.K. Antiochos, A. Phillips, D.S. Spicer, C.R. DeVore, and K.

Shock heating by Fast/Slow MHD waves along plasma loops

Probing Turbulence At and Near CME-driven shocks Using Energetic Particle Spectra Living with a Star Team meeting Sep 18th, 2008 Pasadena, CA Gang Li From.

Initiation of Coronal Mass Ejections: Implications for Forecasting Solar Energetic Particle Storms Ron Moore, Alphonse Sterling, David Falconer, John Davis.

1 Test Particle Simulations of Solar Energetic Particle Propagation for Space Weather Mike Marsh, S. Dalla, J. Kelly & T. Laitinen University of Central.

Coronal Mass Ejection: Initiation, Magnetic Helicity, and Flux Ropes. L. Boundary Motion-Driven Evolution Amari, T., Luciani, J. F., Aly, J. J., Mikic,

Particle spectra at CME-driven shocks and upstream turbulence SHINE 2006 Zermatt, Utah August 3rd Gang Li, G. P. Zank and Qiang Hu Institute of Geophysics.

Y. C.-M. Liu, M. Opher, O. Cohen P.C.Liewer and T.I.Gombosi

George C. Ho1, David Lario1, Robert B. Decker1, Mihir I. Desai2,

Marty Lee Durham, New Hampshire USA

Introduction to Space Weather Interplanetary Transients

Coupled ion acceleration and

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

Solar Wind Transients and SEPs

How does the solar atmosphere connect to the inner heliosphere?

ESS 261 Topics in magnetospheric physics Space weather forecast models ____ the prediction of solar wind speed April 23, 2008.

Introduction to Space Weather

Observations of Magnetic Waves in the Voyager Data Set Marios Socrates Dimitriadis, Charles Smith Introduction Solar wind consists of highly energetic.

Forbush and GCRDs First rigorous experimental observation of Cosmic Ray Flux Decrease was obtained by S. E. Forbush in , after deep statisitcal.

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

Takashi Sakurai National Astronomical Observatory of Japan

Introduction to Space Weather

High-cadence Radio Observations of an EIT Wave

An MHD Model for the Formation of Episodic Jets

Presentation transcript:

Taiyou Zasshikai on May 17, 2004 A Numerical Model of a Coronal Mass Ejection: Shock Development with Implications for the Acceleration of GeV Protons Roussev, I.I., Sokolov, I.V., Forbes, T.G., Gombosi, T.I., Lee, M.A. and Sakai J.I. ApJ, 2004, 605, 73L Taiyou Zasshikai on May 17, 2004 Daikou Shiota

Introduction Coronal mass ejection (CME) Solar energetic particle (SEP) events High energy protons (100MeV) are particularly important Major hazard for spacecraft It has been proposed (e.g., Lee 1997; Reames 1999) these particles are produced by a Fermi process (type A) at a shock in front of the CME (close to the Sun ~10Rsun). However, whether or not such a process is actually feasible has remained uncertain (Tsurutani 2003), because of the lack of knowledge about strength and location of the shock.

Initial configuration Magnetogram data of AR8210 (Wilcox Solar Observatory) Composite synoptic map (Carrington maps for rotation 1935 & 1936) during the period from April through May of 1998 the potential field source surface method (PFSSM; Altschuler et al. 1977) 3D magnetic field + empirical model (Roussev et al. 2003) ↓ time evolution a steady state solar wind

Magnetic configuration and flow pattern

Initiation of CME (Amari et al. 1999, 2000, 2003) converging motions shear motions horizontal boundary motions

Movie

Fast-wave speed Because of this sharp decrease so close to the Sun, the velocity of the ejecta quickly becomes supersonic.

Speed & Trajectories of the flux rope and the shock pure shear motions t=326-365 rapid deceleration due to the formation of the current sheet t=220-326 converging motions t=326-365 rapid acceleration due to loss of equilibrium

3D view

Compression ratio of the shock & Proton cut-off energy a high-energy cutoff for SEPs predicted on the basis of diffusive shock acceleration

Conclusion There has been some controversy in recent years about whether or not diffusive shock acceleration theory can account for the GeV particles observed early in SEP events. By constructing a fully three-dimensional numerical model, which incorporates solar magnetic data and a loss-of-equilibrium mechanism, they have been able to determine that a shock can develop close to the Sun sufficiently strong to account for energetic particles up to 10 GeV.