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

Slides:

Advertisements

Similar presentations

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

Advertisements

THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE CRISM- 2011, Montpellier, 27 June – 1 July, Collaborators:

Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.

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.

Solar flares and accelerated particles

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,

Particle Acceleration in Solar Energetic Particle (SEP) Events and Solar Flares R. P. Lin Physics Department & Space Sciences Laboratory University of.

M. J. Reiner, 1 st STEREO Workshop, March, 2002, Paris.

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

“The Role of Atomic Physics in Spectroscopic Studies of the Extended Solar Corona” – John Kohl “High Accuracy Atomic Physics in Astronomy”, August.

Hard X-Ray Footpoint Motion in Spectrally Distinct Solar Flares Casey Donoven Mentor Angela Des Jardins 2011 Solar REU.

RHESSI 2003 October 28 Time Histories Falling fluxes following the peak Nuclear/511 keV line flux delayed relative to bremsstrahlung Fit to 511 keV line.

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

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

Hard X-rays associated with CMEs H.S. Hudson, UCB & SPRC Y10, Jan. 24, 2001.

Working Group 2 - Ion acceleration and interactions.

More phenomena difficult to observe A MacKinnon. More phenomena difficult to observe synchrotron radiation of positrons: sub-mm observations? inner bremsstrahlung.

Intense Flares Without Solar Energetic Particle Events N. V. Nitta (LMSAL), E. W. Cliver (AFRL), H. S. Hudson (UCB) Abstract: We study favorably located.

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

Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions ITP Santa Barbara, Jan. 18, 2002Hugh.

30-Day Science Plan Angelos Vourlidas, Russ Howard SECCHI Consortium Meeting IAS 8 March 2007.

Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions Yohkoh 10th Jan. 21, 2002Hugh Hudson,

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

From Geo- to Heliophysical Year: Results of CORONAS-F Space Mission International Conference «50 Years of International Geophysical Year and Electronic.

Temporal Variability of Gamma- Ray Lines from the X-Class Solar Flare of 2002 July 23 Albert Y. Shih 1,2, D. M. Smith 1, R. P. Lin 1,2, S. Krucker 1, R.

GLOBAL ENERGETICS OF FLARES Gordon Emslie (for a large group of people)

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

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

STEREO IMPACT Critical Design Review 2002 November 20,21,22 1 LET Performance Requirements Presenter: Richard Mewaldt

8/11/20063 rd SPENVIS USERS WORKSHOP Engineering Models for Galactic Cosmic Rays and Solar Protons: Current Status Stephen Gabriel Professor of Aeronautics.

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

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.

The Sun and the Heliosphere: some basic concepts…

Solar System Missions Division Solar Orbiter Next major Solar and Heliospheric mission ESA ILWS flagship Now with the Inner Heliospheric Sentinels.

The Relation between Soft X-ray Ejections and Hard X-ray Emission on November 24 Flare H. Takasaki, T. Morimoto, A. Asai, J. Kiyohara, and K. Shibata Kwasan.

RHESSI and Radio Imaging Observations of Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD G. Trottet, Observatoire.

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.

Observation of impulsive Solar Flares with the Fermi Large Area Telescope ! Fermi LAT and GBM Collaborations.

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,

ACE Page 1 ACE ACE PresentorInstitution. ACE Page 2 ACE Mass Fractionation in the Composition of Solar Energetic Particles Although it is well known that.

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

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

Studies on the 2002 July 23 Flare with RHESSI Ayumi ASAI Solar Seminar, 2003 June 2.

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.

Lessons for STEREO - learned from Helios Presented at the STEREO/Solar B Workshop, Rainer Schwenn, MPS Lindau The Helios.

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.

The Suprathermal Tail Properties are not well understood; known contributors Heated solar wind Interstellar and inner source pickup ions Prior solar and.

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

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

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

Analysis of 3 and 8 April 2010 Coronal Mass Ejections and their Influence on the Earth Magnetic Field Marilena Mierla and SECCHI teams at ROB, USO and.

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,

An Introduction to Observing Coronal Mass Ejections

Physics of Solar Flares

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.

Marina Battaglia, FHNW Säm Krucker, FHNW/UC Berkeley

Ian Richardson HILARY CANE Bruny Island and Tycho von Rosenvinge

LET Performance Requirements Presenter: Richard Mewaldt

N. Giglietto (INFN Bari) and

Introduction to Space Weather Interplanetary Transients

A SOLAR FLARE is defined as a

Corona Mass Ejection (CME) Solar Energetic Particle Events

Difficult to relate EIT waves to other phenomena due to cadence

Relative abundances of quiet-time suprathermal ions at 1 AU

SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS

High-cadence Radio Observations of an EIT Wave

Transition Region and Coronal Explorer (TRACE)

Presentation transcript:

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

Solar Energetic Particle (SEP) events observed in the Interplanetary Medium (IPM): * Large (L)SEP events (~tens per year at solar maximum) - dominated by >10 MeV protons normal coronal composition and charge states - associated with fast Coronal Mass Ejections (CMEs) large flares (sometimes missing) gradual soft X-ray bursts * Electron - 3 He-rich SEP events (~10 3 s per year at solar maximum) - dominated by ~ keV electrons and ~ MeV/nuc 3 He enhanced Fe, Mg, Si, S; high charge states - associated with small flares/coronal microflares Type III radio bursts impulsive soft X-ray bursts

π 0 Decay Nonthermal Bremsstrahlung Thermal Bremsstrahlung Composite Solar Flare Spectrum Positron and Nuclear Gamma-Ray lines T = 2 x 10 7 K T = 4 x 10 7 K

Results Comparison: 23 July 2003, 00:30: :30:20 White: Johns & Lin (1992) Red: Piana et al. 0th order regularization

Contours of an 8'' FWHM Gaussian source with its associated albedo patch. (factor of 2 contours) The green contours show the levels of integrated albedo flux. The 2 nd green (~35''x100'') contour contains 75% of the albedo flux, assumed here to be 50% of the primary source flux. WITH IMAGING DOWN TO THE 1% LEVEL AND ZERO NOISE RHESSI-NESSI-II March 2004 E J Schmahl (2004) 6% 3% 1.5%

Pileup Corrections: Use only those photons for which the live-time > 80% No albedo With albedo

Active Region 9901

Coronal Source keV keV14-16 keV

Temperature Distribution (I) (04/15 23:11:00 UT)

(From Ohyama & Shibata 1998) Cartoon of Flare Model

(From Lin 2003) Flux Rope Model

Inner Heliosphere is unexplored Phenomena of critical importance to LWS (solar wind and CME origin and evolution, SEP acceleration) occur in the Inner Heliosphere No in situ measurements inside 0.3 AU and only Helios (two decades ago) between 0.3 and ~1 AU New diagnostics and technology available for inner heliosphere missions Multi-point measurements with a range of radial distances and longitudes (latitudes) desired

Missions being developed: STEREO Solar B Solar Dynamics Observatory Missions being studied: Solar Orbiter (ESA) - ~0.2 AU Solar Probe - ~3 solar radii Inner Heliospheric Sentinels - ?