Particles integrate the field H.S. Hudson UC Berkeley.

Slides:



Advertisements
Similar presentations
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.
Advertisements

Magnetic Reconnection Across the HCS Mark Moldwin UM and Megan Cartwright UC-Berkeley Isradynamics April 2010 With thanks to Mark Linton at NRL Linton.
Single particle motion and trapped particles
Solar Energetic Particles and Shocks. What are Solar Energetic Particles? Electrons, protons, and heavier ions Energies – Generally KeV – MeV – Much less.
Bastille Day 2000 Solar Energetic Particles Event: Ulysses observations at high heliographic latitudes M. Zhang Florida Institute of Technology.
Five Spacecraft Observations of Oppositely Directed Exhaust Jets from a Magnetic Reconnection X-line Extending > 4.3 x 10 6 km in the Solar Wind Gosling.
Electron Acceleration at the Solar Flare Reconnection Outflow Shocks Gottfried Mann, Henry Aurass, and Alexander Warmuth Astrophysikalisches Institut Potsdam,
Hard X-rays associated with CMEs H.S. Hudson, UCB & SPRC Y10, Jan. 24, 2001.
The mystery of the MISSING MOMENTUM H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group, Glasgow.
Coronal radiation belts? H. S. Hudson Space Sciences Lab, UC Berkeley.
Energetic neutral atoms from solar flares H. S. Hudson SSL, UC Berkeley.
Solar Energetic Particle Production (SEPP) Mission Primary Contacts: Robert P. Lin (UC Berkeley), John L. Kohl (Harvard-Smithsonian CfA) Primary Science.
Solar evidence for magnetic reconnection H. S. Hudson Space Sciences Lab, UC Berkeley.
Energetic Particles in the Quiet Corona A. MacKinnon 1,2, M. DeRosa 3, S. Frewen 2, & H. Hudson 2 1 University of Glasgow, 2 Space Sciences Laboratory,
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 MURI, June 2003 H.S. Hudson Tracing SEPs from Earth to Sun H. Hudson.
PTA, September 21, 2005 Solar flares in the new millennium H.S. Hudson Space Sciences Lab, UC Berkeley.
Coronal radiation belts? H. S. Hudson Space Sciences Lab, UC Berkeley Elliot (1973) cartoon, from
Coronal hard X-rays prior to RHESSI H. S. Hudson Space Sciences Lab, UC Berkeley.
RHESSI OBSERVATIONS OF FLARE FOOTPOINTS AND RIBBONS H. Hudson and M. Fivian (SSL/UCB)
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.
In-situ Observations of Collisionless Reconnection in the Magnetosphere Tai Phan (UC Berkeley) 1.Basic signatures of reconnection 2.Topics: a.Bursty (explosive)
Space Science MO&DA Programs - December Page 1 SS Interplanetary Propagation of Ions From Impulsive Solar Flares: ACE/ULEIS Data Impulsive solar.
Reinisch_ Lecture_6. reinisch_ Nonuniform B Field Gradient-B drift.
Modeling of solar radiation belts S. Frewen 1, M. DeRosa 2, H. Hudson 1, and A. MacKinnon 3 Abstract: Stable particle trapping in the complicated magnetic.
Physics of fusion power Lecture 14: Collisions / Transport.
CISM SEP Modeling Background The major SEP events come from the CME-generated coronal and interplanetary shock(s) These “gradual”events can have a “prompt”
Coronal Hard X-rays Come of Age H. S. Hudson SSL, UC Berkeley.
DOPPLER DOPPLER A Space Weather Doppler Imager Mission Concept Exploration Science Objectives What are the most relevant observational signatures of flare,
Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,
Magnetospheric Morphology Prepared by Prajwal Kulkarni and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global.
Microflares now, major flares soon H.S. Hudson Space Sciences Lab, UC Berkeley.
Coronal radiation belts H. S. Hudson 1, M. DeRosa 2, & A. MacKinnon 3 1 Space Sciences Lab, UC Berkeley; 2 LMSAL; 3 University of Glasgow Abstract: We.
Physics of fusion power
Physics of fusion power Lecture 7: particle motion.
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
Space Weather Alice Hirsh International Studies and Economics College of Arts and Sciences.
By: Kiana and Meagan. Purpose  To measure solar magnetic fields  To understand how energy generated by magnetic-field changes in the lower solar atmosphere.
Introduction to Space Weather
IHY Workshop A PERSONAL VIEW OF SOLAR DRIVERS for Solar Wind Coronal Mass Ejections Solar Energetic Particles Solar Flares.
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.
Motion in a constant uniform magnetic field Section 21.
Plasmas. The “Fourth State” of the Matter The matter in “ordinary” conditions presents itself in three fundamental states of aggregation: solid, liquid.
Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,
SUN, EARTH AND SPACE. THE SUN CLOSE UP: INSIDE AND OUT.
THE EARTH’S MAGNETIC FIELD Note; The geographical north pole acts like the south pole of a magnet.
Space Environment SSE-120 Please type in your questions and raise your hand so we can answer it during class.
Ion pickup and acceration in magnetic reconnection exhausts J. F. Drake University of Maryland M. Swisdak University of Maryland T. Phan UC Berkeley E.
1 Space technology course : Space Radiation Environment and its Effects on Spacecraft Components and Systems Space radiation environment Space Radiation.
Solar Astronomy Space Science Lab 2008 Pisgah Astronomical Research Institute.
The Solar Wind. The Sun is not a quiet place. Disturbances in the Sun’s magnetic field create Sunspots.
1 Test Particle Simulations of Solar Energetic Particle Propagation for Space Weather Mike Marsh, S. Dalla, J. Kelly & T. Laitinen University of Central.
An Introduction to Observing Coronal Mass Ejections
ESS 154/200C Lecture 15 The Inner Magnetosphere II
Solar Flare Energy Partition into Energetic Particle Acceleration
THE SUN AS AN ENERGY SOURCE
The Sun: Portrait of a G2V star
Corona Mass Ejection (CME) Solar Energetic Particle Events
Alexei Struminsky1,2  1 Space Research Institute
Solar and Heliospheric Physics
Overview of the Sun Jie Zhang Art Poland
What is the sun? What is the structure of the sun?
Heliospheric/ISTP Missions Science Highlights
SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS
The Sun.
Evidence for magnetic reconnection in the high corona
Slit and Slot Interchange
CORONAL MASS EJECTIONS
Presentation transcript:

Particles integrate the field H.S. Hudson UC Berkeley

Tutorial 0 Only particle measurements can really show field lines Velocity distribution functions show that the plasma invariably has a tail of energetic particles

Tutorial 1 Larmor radii Debye lengths Inertial scales Ranges

Tutorial 2 Adiabatic invariants of motion - Mirror (OK in corona) - Bounce (OK in corona sometimes) - Drift (Doesn’t work in corona)

Tutorial 3 Non-adiabatic motions (guiding-center drifts) Electrons in space Flares, jets, etc.

Conclusions Energetic particles define field lines “Marker” flares/type IIIs occur Energetic electrons detectable at 1 A.U. can originate deep in the atmosphere, and arrive immediately Therefore, the particles can provide an exact integral of the corona/SW field

Program Link heliospheric particle measurements with what happens at the Sun - Direct connectivity for open field lines - Morphology of active regions with radio signatures Compare this new information about connectivity with what we learn about coronal B Answer the question, “Can we close the universe with magnetic energy?”