What role do energetic particles present in the dayside cusp play in magnetospheric processes? THEODORE A. FRITZ Center for Space Physics at Boston University.

Slides:



Advertisements
Similar presentations
UAH The Spinning Terrella Experiment: Lab Analog for Earth's Magnetosphere Robert Sheldon 1, Eric Reynolds 2 1 National Space Science and Technology Center,
Advertisements

First composition measurements of energetic neutral atoms A. T. Y. Lui et al., GRL, Vol 23, pages: , 1996.
Evidence at Saturn for an Inner Magnetospheric Convection Pattern, Fixed in Local Time M. F. Thomsen (1), R. L. Tokar (1), E. Roussos (2), M. Andriopoulou.
Formation of the Magnetosphere 1 Solar Wind. Formation of the Magnetosphere 2 Solar Wind Bow Shock Magnetosheath.
Single particle motion and trapped particles
Magnetopause flow vortices revealed during high speed solar wind streams Mona Kessel (NASA GSFC), Yaireska Collado-Vega (University of Puerto Rico), Xi.
Radiation Belt Loss at the Magnetopause T. G. Onsager, J. C. Green, H. J. Singer, G. D. Reeves, S. Bourdarie Suggest a pitch-angle dependence of magnetopause.
Cusp Radiation Source: A Challenge for Theory and Simulation Jiasheng Chen, Theodore A. Fritz, Katherine E. Whitaker, Forrest S. Mozer, and Robert B. Sheldon.
Auxiliary slides. ISEE-1 ISEE-2 ISEE-1 B Locus of  = 90 degree pitch angles Will plot as a sinusoid on a latitude/longitude projection of the unit.
Solar wind-magnetosphere coupling Magnetic reconnection In most solar system environments magnetic fields are “frozen” to the plasma - different plasmas.
Storm-Time Dynamics of the Inner Magnetosphere: Observations of Sources and Transport Michelle F. Thomsen Los Alamos National Laboratory 27 June 2003.
Physics of fusion power Lecture 8: Conserved quantities / mirror / tokamak.
CISM Radiation Belt Models CMIT Mary Hudson CISM Seminar Nov 06.
Or A Comparison of the Magnetospheres between Jupiter and Earth.
Reinisch_ Solar Terrestrial Relations (Cravens, Physics of Solar Systems Plasmas, Cambridge U.P.) Lecture 1- Space Environment –Matter in.
CISM Advisory Council Meeting 4 March 2003 Magnetospheric Modeling Mary K. Hudson and the CISM Magnetospheric Modeling Team.
Observations of Open and Closed Magnetic Field Lines at Mars: Implications for the Upper Atmosphere D.A. Brain, D.L. Mitchell, R. Lillis, R. Lin UC Berkeley.
Solar system science using X-Rays Magnetosheath dynamics Shock – shock interactions Auroral X-ray emissions Solar X-rays Comets Other planets Not discussed.
Magnetospheric Morphology Prepared by Prajwal Kulkarni and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global.
1 Dynamic Motion of Bow Shock and Magnetopause Observed by THEMIS Hui Zhang (BU) Q.-G. Zong (Umass Lowell) D. G. Sibeck (GSFC) T. A. Fritz (BU)
ESS 7 Lectures 10, 11 and 12 October 22, 24, and 27 The Magnetosphere.
Physics of fusion power Lecture 7: particle motion.
Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland
Benoit Lavraud CESR/CNRS, Toulouse, France Uppsala, May 2008 The altered solar wind – magnetosphere interaction at low Mach numbers: Magnetosheath and.
Introduction to Space Weather
1 Cambridge 2004 Wolfgang Baumjohann IWF/ÖAW Graz, Austria With help from: R. Nakamura, A. Runov, Y. Asano & V.A. Sergeev Magnetotail Transport and Substorms.
Magnetosphere-Ionosphere coupling processes reflected in
Computational Model of Energetic Particle Fluxes in the Magnetosphere Computer Systems Yu (Evans) Xiang Mentor: Dr. John Guillory, George Mason.
1 The Inner Magnetosphere Nathaniel Stickley George Mason University.
Localized Thermospheric Energy Deposition Observed by DMSP Spacecraft D. J. Knipp 1,2, 1 Unversity of Colorado, Boulder, CO, USA 2 High Altitude Observatory,
Earth’s Magnetosphere — A very quick introduction Weichao Tu - LASP of CU-Boulder CEDAR-GEM Joint Workshop - Santa Fe, NM - 06/26/2011.
Ionospheric Current and Aurora CSI 662 / ASTR 769 Lect. 12 Spring 2007 April 24, 2007 References: Prolss: Chap , P (main) Tascione: Chap.
Response of the Magnetosphere and Ionosphere to Solar Wind Dynamic Pressure Pulse KYUNG SUN PARK 1, TATSUKI OGINO 2, and DAE-YOUNG LEE 3 1 School of Space.
ESS 7 Lecture 13 October 29, 2008 Substorms. Time Series of Images of the Auroral Substorm This set of images in the ultra-violet from the Polar satellite.
E.E. Antonova1,2, I.P. Kirpichev2,1, Yu.I. Yermolaev2
Relating the Equatorward Boundary of the Diffuse Redline Aurora to its Magnetospheric Counterpart Grant, Jeff 1 ; Donovan, Eric 1 ; Spanswick, Emma 1 ;
PARTICLES IN THE MAGNETOSPHERE
WG2 Summary Broke into ring current/plasmasphere and radiation-belt subgroups RING CURRENT Identified events for addressing science questions What is the.
NASA NAG Structure and Dynamics of the Near Earth Large-Scale Electric Field During Major Geomagnetic Storms P-I John R. Wygant Assoc. Professor.
17th Cluster workshop Uppsala, Sweden , May 12-15, 2009
The Geomagnetic Cusps: Magnetic Topology and Physical Processes Antonius Otto Thanks to: Eric Adamson, Katariina Nykyri, Julia Pilchowski, Jason McDonald.
Magnetospheric Current System During Disturbed Times.
CAMMICE Science Report March 31, 2006 There will be two sections to the report: 1.A discussion on the inter-comparison of the responses of the MICS, Hydra,
The large scale convection electric field, ring current energization, and plasmasphere erosion in the June 1, 2013 storm Scott Thaller Van Allen Probes.
MULTI-INSTRUMENT STUDY OF THE ENERGY STEP STRUCTURES OF O + AND H + IONS IN THE CUSP AND POLAR CAP REGIONS Yulia V. Bogdanova, Berndt Klecker and CIS TEAM.
Particle precipitation has been intensely studied by ionospheric and magnetospheric physicists. As particles bounce along the earth's magnetic fields they.
© Research Section for Plasma and Space Physics UNIVERSITY OF OSLO Daytime Aurora Jøran Moen.
SEPT/STEREO Observations of Upstream Particle Events: Almost Monoenergetic Ion Beams A. Klassen, R. Gomez-Herrero, R. Mueller-Mellin and SEPT Team, G.
ASEN 5335 Aerospace Environments -- Magnetospheres 1 As the magnetized solar wind flows past the Earth, the plasma interacts with Earth’s magnetic field.
Multi-Fluid/Particle Treatment of Magnetospheric- Ionospheric Coupling During Substorms and Storms R. M. Winglee.
Lecture 15 Modeling the Inner Magnetosphere. The Inner Magnetosphere The inner magnetosphere includes the ring current made up of electrons and ions in.
On-Line Visualization Ring Current / Radiation Belt.
A Global Hybrid Simulation Study of the Solar Wind Interaction with the Moon David Schriver ESS 265 – June 2, 2005.
SECAS Dec 01 MISSIONS: POLAR, WIND, GEOTAIL, CLUSTER Jim Sharber MISSION STATUS.
Challenges The topological status of the magnetosphere: open or closed? Driver(s) of ionospheric sunward flow Source(s) of NBZ currents Key problem: are.
Plasma Wave Excitation Regions in the Earth’s Global Magnetosphere
ESS 154/200C Lecture 15 The Inner Magnetosphere II
Paul Song Center for Atmospheric Research
The Magnetosphere Feifei Jiang, UCLA
Characterization of Field Line Topologies Near the Magnetopause Using Electron Pitch Angle Measurements D. S. Payne1, M. Argall1, R. Torbert1, I. Dors1,
Single particle motion and trapped particles
Introduction to Space Weather Interplanetary Transients
The Physics of Space Plasmas
Introduction to Space Weather
Penetration Jet DMSP F April MLT
Solar Wind-Magnetosphere Interaction: Reconnection and IMF Dependence
Magnetosphere: Bow Shock Substorm and Storm
Dynamic Coupling between the Magnetosphere and the Ionosphere
On Strong Coupling between the Harang Reversal Evolution and Substorm Dynamics: A Synthesis of SuperDARN, DMSP and IMAGE Observations Shasha Zou1, Larry.
Magnetosphere: Structure and Properties
Presentation transcript:

What role do energetic particles present in the dayside cusp play in magnetospheric processes? THEODORE A. FRITZ Center for Space Physics at Boston University Polar PI Telecon March 7, 2008 Thanks to Jiasheng Chen, Jon Niehof, Mike Klida, Kate Whitaker, Brian Walsh, Charlotte Wong, Zhang Hui, the Polar CAMMICE team and the Cluster RAPID team

The McIlwain E3 model does not look anything like the classical ideas of the origin of the cross- tail electric field Lyons and Williams, 1984 What does this have to do with the cusp?

The conclusion to draw from this: Within the cusp there appear to be embedded regions containing diamagnetic cavities (CDC). Within the CDCs the field and particle pressures are strongly anti- correlated whereas within the cusp outside the CDCs the anti-correlation no longer holds. Within the cusp, ions with energies >20 keV up to many 100s of keV (CEP) are present only in those portions of the cusp associated with diamagnetic cavities (CDC). Polar sees CDC that are very large (>6 R E and lasting for hours) At the Polar team meeting in October I presented strong evidence from a combination of Polar, Cluster, and ISEE that the CEPs are energized locally in the cusp from a source population of shocked solar wind ions and up-flowing ionospheric ions.

These CEP/CDC regions are present all of the time independent of solar wind and IMF conditions—the only criteria from the perspective of the Polar satellite being that a satellite must be in the right position to observe them. These CEP particles have pitch angle distributions in which the anti-field aligned direction (  =180 0 ) is full with the opposite direction basically empty. These particles will paint the magnetopause with a layer of energetic particles. The questions that now remain are what effects, if any, these particles have on magnetospheric processes? Are they the source of the ring current via gradient and curvature drifts to the nightside inner magnetosphere? Do these particles create, via charge separation, the cross polar-cap potential?

Conclusions Since these particles are mostly on “open” field lines they will paint the magnetopause with a layer of energetic particles and will populate the upstream medium when an appropriate IMF orientation is present. In addition many of these energetic ions in the cusp will gradient and curvature drift, --ions to the west and electrons to the east, -- separating and drifting along what we have described as a Shabansky orbit that will carry the particles to the equatorial plane around dusk and dawn. These energetic particles on the magnetopause will reenter the magnetosphere -- ions along the dawn flank and electrons along the dusk flank.

Only slight imbalances of these charges is sufficient to establish large charge-separation electric fields. Such charge-separation electric fields can explain most of the features of the McIlwain E3 model.

The E3 model of Carl E. McIlwain was based on plasma measurements at 6.6 R E Note the strong radial field in the post- midnight/pre-dawn sector and a dawn to dusk field only near the midnight sector. McIlwain, 1976