SSL UC Berkeley 2010 June ACE/SOHO/STEREO/Wind Workshop When and Where are Impulsive SEPs Accelerated? Linghua Wang, Bob Lin, S ä m Krucker Space Sciences.

Slides:

Advertisements

Similar presentations

SHINE 2008 Introduction Energetic ElectronsFluence AnalysisSummary George C. Ho and Glenn M. Mason The Johns Hopkins University Applied Physics Laboratory,

Advertisements

THE IMPULSIVE X-RAY RESPONSE IN FLARE FOOTPOINTS TOMASZ MROZEK WROCLAW UNIWERSITY ASTRONOMICAL INSTITUTE POLAND.

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

On the link between the solar energetic particles and eruptive coronal phenomena On the link between the solar energetic particles and eruptive coronal.

The Physics of Solar Flares Examining Solar Flares and Radio Bursts By Caylin Mendelowitz and Claire Rosen.

R. P. Lin Physics Dept & Space Sciences Laboratory University of California, Berkeley The Solar System: A Laboratory for the Study of the Physics of Particle.

Hot Precursor Ejecta and Other Peculiarities of the 2012 May 17 Ground Level Enhancement Event N. Gopalswamy 2, H. Xie 1,2, N. V. Nitta 3, I. Usoskin 4,

X-ray Emission due to Charge Exchange between Solar Wind and Earth Atmosphere on September Hironori Matsumoto (Kobayashi-Maskawa Institute, Nagoya.

The Focusing Optics X-ray Solar Imager (FOXSI) Steven Christe 1, S. Krucker 2, L. Glesener 2, S. Ishikawa 3, B. Ramsey 4, T. Takahashi 3, R.P. Lin 2 1.

Low-Energy Coronal Sources Observed with RHESSI Linhui Sui (CUA / NASA GSFC)

Strength of Coronal Mass Ejection- driven Shocks Near the Sun and Its Importance in Predicting Solar Energetic Particle Events Chenglong Shen 1, Yuming.

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

CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM WORKSHOP 1 Observations Questions.

Flare footpoints and ribbons: The impulsive phase H.S. Hudson Space Sciences Lab, UC Berkeley.

Solar and Stellar Flares Hugh S. Hudson SSL, UC Berkeley 1 May

Working Group 2 - Ion acceleration and interactions.

Characterizing Thermal and Non- Thermal Electron Populations in Solar Flares Using RHESSI Amir Caspi 1,2, Säm Krucker 2, Robert P. Lin 1,2 1 Department.

Relationships between flares and CMEs H.S. Hudson Space Sciences Lab, UC Berkeley.

Hard X-ray sources in the solar corona H.S. Hudson Space Sciences Lab, UC Berkeley.

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

Coronal IP Shocks Nat Gopalswamy NASA/GSFC Elmau CME Workshop, 2003 February 7 Plenary talk Sun Earth.

SEPs and Solar Radio Bursts S. Krucker and H. Hudson Time-of-flight analysis of SEP propagation Connectivity of the SEP field lines SIRA relevance.

Space Science MO&DA Programs - December Page 1 SS Interplanetary Propagation of Ions From Impulsive Solar Flares: ACE/ULEIS Data Impulsive solar.

1 Statistical determination of chromospheric density structure using RHESSI flares Pascal Saint-Hilaire Space Sciences Lab, UC Berkeley RHESSI Workshop.

SSL UC Berkeley 2010 June ACE/SOHO/STEREO/Wind Workshop Interplanetary Propagation of Solar Impulsive Energetic Electrons Linghua Wang, Bob Lin and S ä.

Hard X-ray Diagnostics of Solar Eruptions H. Hudson SSL, UC Berkeley and U. Of Glasgow.

Coronal Hard X-rays Come of Age H. S. Hudson SSL, UC Berkeley.

Late-phase hard X-ray emission from flares The prototype event (right): March 30, 1969 (Frost & Dennis, 1971), a very bright over-the-limb event with a.

Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,

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

Solar Origin of energetic particle events Near-relativistic impulsive electron events observed at 1 AU M. Pick, D. Maia, S.J. Wang, A. Lecacheux, D. Haggery,

SMESE: a French/Chinese Solar “SMEX” H.S. Hudson Space Sciences Lab, UC Berkeley.

Long-Lasting 3 He-Rich Solar Energetic Particle Sources R. Bučík, D. E. Innes, U. Mall, A. Korth (MPS) G. M. Mason (JHU) R. Gómez-Herrero (UAH) STEREO.

The Sun and the Heliosphere: some basic concepts…

RHESSI Microflares Steven Christe 1,2, Säm Krucker 2, Iain Hannah 3, R. P. Lin 1,2 1 Physics Department, University of California at Berkeley 2 Space Sciences.

Sinaia, September 6-10, Berndt Klecker Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Workshop on Solar Terrestrial Interactions.

Evidence of Chromospheric Evaporation in a Neupert-type Flare NING Zongjun Purple Mountain Observatory, China.

IHY Workshop A PERSONAL VIEW OF SOLAR DRIVERS for Solar Wind Coronal Mass Ejections Solar Energetic Particles Solar Flares.

Relation between Type II Bursts and CMEs Inferred from STEREO Observations N. Gopalswamy, W. Thompson, J. Davila, M. Kaiser NASA Goddard Space Flight Center,

Coronal hard X-ray sources and associated decimetric/metric radio emissions N. Vilmer D. Koutroumpa (Observatoire de Paris- LESIA) S.R Kane G. Hurford.

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

Elemental Abundance variations of the Suprathermal Heavy Ion Population over solar cycle 23 M. Al Dayeh, J.R. Dwyer, H.K. Rassoul Florida Institute of.

Radio diagnostics of electron acceleration in the corona and in the IP medium Radio observations of the late/gradual/second phase of flares: implications.

Coronal Sources of Impulsive Fe-Rich Solar Energetic Particle Events S. W. Kahler AFRL Space Vehicles Directorate, Kirtland AFB, NM, USA D. V. Reames IPST,

LASCO C2 Jan 24, 2006, www image Future progress understanding Solar Energetic Particles Glenn Mason, JHU/APL 10th RHESSI Workshop Annapolis, MD August.

1 20 January 2005: Session Summary SHINE 2006 Zermatt, Utah, 31 July - 4 August Invited Talks Riley: what was the Alfven speed in the corona at.

Project: Understanding propagation characteristics of heavy ions to assess the contribution of solar flares to large SEP events Principal Investigator:

He + Increase in SEP Events with a High Source Temperature and Implication for Acceleration Site ICRC, 2011, Beijing Z. Guo; E. Moebius; M. Popecki Space.

1 SEP “Campaign Events” for SHINE 2003 Question: Can we identify solar/interplanetary factors that drive SEP spectral and compositional variability at.

SHINE SEP Campaign Events: Detailed comparison of active regions AR9906 and AR0069 in the build-up to the SEP events of 21 Apr 2002 and 24 Aug 2002 D.

SH 51A-02 Evolution of the coronal magnetic structures traced by X-ray and radio emitting electrons during the large flare of 3 November 2003 N.Vilmer,

The Space Weather Week Monique Pick LESIA, Observatoire de Paris November 2006.

Characterizing Thermal and Non- Thermal Electron Populations in Solar Flares Using RHESSI Amir Caspi 1,2, Säm Krucker 2, Robert P. Lin 1,2 1 Department.

Tasks: Pasadena, 9/18/08. Exponential Rollovers Origin of double power laws? Need analysis and simulation. Correlating E and Q/A dependence; explore different.

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

Multi-spacecraft observations of solar energetic electron events during the rising phase of solar cycle 24 W. Droege 1, R. Gomez-Herrero 2, J. Kartavykh.

Coronal X-ray Emissions in Partly Occulted Flares Paula Balciunaite, Steven Christe, Sam Krucker & R.P. Lin Space Sciences Lab, UC Berkeley limb thermal.

Karl-Ludwig Klein

Observations –Morphology –Quantitative properties Underlying Physics –Aly-Sturrock limit Present Theories/Models Coronal Mass Ejections (CME) S. K. Antiochos,

1 SEP Timing Studies: An Excruciatingly Brief Review Allan J. Tylka US Naval Research Laboratory, Washington DC SHINE 2006 Where was the CME when the SEPs.

Coronal hard X-ray sources and associated radio emissions N. Vilmer D. Koutroumpa (Observatoire de Paris- LESIA; Thessaloniki University) S.R Kane G. Hurford.

Interplanetary proton and electron enhancements associated with radio-loud and radio-quiet CME-driven shocks P. Mäkelä 1,2, N. Gopalswamy 2, H. Xie 1,2,

Elemental Abundance variations of the Suprathermal Heavy Ion Population over solar cycle 23 M. Al Dayeh, J.R. Dwyer, H.K. Rassoul Florida Institute of.

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

Modeling the SEP/ESP Event of December 13, 2006

Solar Flare Energy Partition into Energetic Particle Acceleration

Alexei Struminsky1,2 1 Space Research Institute

Coronal and interplanetary radio emission as a tracer of solar energetic particle propagation Karl-Ludwig Klein (F Meudon)

Conveners: M. A. Dayeh (SwRI), R. Bucik (MPS/UG), and C. Salem (UCB)

Nonthermal Electrons in an Ejecta Associated with a Solar Flare

Presentation transcript:

SSL UC Berkeley 2010 June ACE/SOHO/STEREO/Wind Workshop When and Where are Impulsive SEPs Accelerated? Linghua Wang, Bob Lin, S ä m Krucker Space Sciences Lab, UC Berkeley and G. Mason Applied Physics Lab, JHU

The red curves are the best fits to the rise of observations.

Red triangles: Ion injection profiles Black triangles: Electron injection profiles Ion Delay: 48  21 mins Type III

0.92 keV electrons ~ 0.060c 1.67 MeV/nuc ~ 0.060c

Averaged delay of ion release: 1.2±0.2 hours delay of ion release = ion release time – low (  6-9 keV) energy electron release time

All have a type III burst, but only one has a type II burst. Three possibly have a small GOES SXR flare. Nine have SOHO/LASCO observations. All the nine have a west-limb CME.

CMEs related to electron/ 3 He-rich SEPs (red crosses) average CME speed average width (excluding halo CMEs) CMEs related to 3 He-rich events are fast and rather narrow.

Summary Double electron injections at the Sun: one at energies below 6-9 keV, 9.1 ±2.4 min before the release of type III burst (the source of type III burst) a second at energies above 9-13 keV, 8.2±0.6 min (delayed) after type III burst. Delayed solar injection of 3 He-rich ions: 1.2 ± 0.2 hr w.r.t low-energy (  6-9 keV) e − s ; 0.9 ± 0.2 hr w.r.t high-energy (≥9-13 keV) e − s ; suggesting a later acceleration.

These events have no strong SXR flares. Among nine events with the SOHO/LASCO observations, all have a fast west-limb CME (>570 km/s). The majority of the fast CMEs are narrow delayed (~1 hour) ion acceleration - CMEs ( ~4 Rs at the ion release time) hardly produce high charge states by stripping - electrons waves accelerate 3 He-rich ions ~ 1 hour delay (???) ; ~ Altitudes > ~ 0.5 Rs

Nτ A ~ – s·cm -3 [e.g., Kocharov et al., 2000; Kartavykh et al., 2006], where N is the plasma density and τ A is the acceleration time scale. If τ A is ~ 1 hour, then N would be ~ 10 6 – 10 7 cm -3, corresponding to altitudes >~ 0.5 Rs, high in the corona. The acceleration mechanism is likely the resonance with wave modes that can preferentially heat/accelerate 3 He and heavy ions due to their unique charge-to-mass ratios [e.g., Fisk, 1978; Temerin & Roth, 1992; Roth & Temerin, 1997; Miller & Viñas, 1993; Miller, 1998; Liu et al., 2006; Paesold et al., 2003] - Interplanetary scattering??