Cusp Radiation Source: A Challenge for Theory and Simulation Jiasheng Chen, Theodore A. Fritz, Katherine E. Whitaker, Forrest S. Mozer, and Robert B. Sheldon.

Slides:

Advertisements

Similar presentations

Generation of the transpolar potential Ramon E. Lopez Dept. of Physics UT Arlington.

Advertisements

Electron Acceleration in the Van Allen Radiation Belts by Fast Magnetosonic Waves Richard B. Horne 1 R. M. Thorne 2, S. A. Glauert 1, N. P. Meredith 1.

ESS 7 Lecture 14 October 31, 2008 Magnetic Storms

Low-Frequency Waves Excited by Newborn Interstellar Pickup Ions H + and He + at 4.5 AU Charles W. Smith, Colin J. Joyce, Philip A. Isenberg, Neil Murphy,

Weaker Solar Wind Over the Protracted Solar Minimum Dave McComas Southwest Research Institute San Antonio, TX With input from and thanks to Heather Elliott,

Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS,

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.

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

Simulated Response of the Magnetosphere-Ionosphere System to Empirically Regulated Ionospheric H + Outflows W Lotko 1,2, D Murr 1, P Melanson 1, J Lyon.

Simulated Response of the Magnetosphere-Ionosphere System to Empirically Regulated Ionospheric H + Outflows W Lotko 1,2, D Murr 1, P Melanson 1, J Lyon.

State Key Laboratory of Space Weather An inter-hemisphere asymmetry of the cusp region against the geomagnetic dipole tilt Jiankui Shi Center for Space.

O. M. Shalabiea Department of Physics, Northern Borders University, KSA.

CISM Radiation Belt Models CMIT Mary Hudson CISM Seminar Nov 06.

Reinisch_ Solar Terrestrial Relations (Cravens, Physics of Solar Systems Plasmas, Cambridge U.P.) Lecture 1- Space Environment –Matter in.

Lecture 3 Introduction to Magnetic Storms. An isolated substorm is caused by a brief (30-60 min) pulse of southward IMF. Magnetospheric storms are large,

In-situ Observations of Collisionless Reconnection in the Magnetosphere Tai Phan (UC Berkeley) 1.Basic signatures of reconnection 2.Topics: a.Bursty (explosive)

What DMSP Data Tell us About the Thermosphere Response to Solar Wind Forcing Delores Knipp CU Aerospace Engineering Sciences and NCAR HAO With Assistance.

Stormtime plasmasheet access to the inner magnetosphere: evidence for an internal source S. R. Elkington LASP, University of Colorado, Boulder A. A. Chan,

Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland

A Scaleable Model of Magnetospheric Radiation Belt Dynamics Robert Sheldon, Wheaton College TOP SIDE t=0 Double Dipole,

The Physics of Space Plasmas William J. Burke 14 November 2012 University of Massachusetts, Lowell Magnetic Storms and Substorms.

D. Sibeck, R. Millan, H. Spence

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

Does Fermi Acceleration of account for variations of the fluxes of radiation belt particles observations at low altitudes during geomagnetic storms? J.

Finite Gyroradius Effect in Space and Laboratory 1. Radiation belt (Ring current) 2. Auroral phenomena (Substorm current) 3. Shock acceleration and upstream.

20 September 2005Double Star -Cluster Noordwijk Sept WBD Studies of AKR: Coordinated Observations of Aurora and the SAKR – Ion Hole Connection R.

The energetics of the slow solar wind Leon Ofman, Catholic University of America, NASA GSFC, Code 612.1, Greenbelt, MD 20771, USA

Large-Amplitude Electric Fields Associated with Bursty Bulk Flow Braking in the Earth’s Plasma Sheet R. E. Ergun et al., JGR (2014) Speaker: Zhao Duo.

Localized Thermospheric Energy Deposition Observed by DMSP Spacecraft D. J. Knipp 1,2, 1 Unversity of Colorado, Boulder, CO, USA 2 High Altitude Observatory,

Large electric fields near the nightside plasmapause observed by the Polar spacecraft K.-H. Kim 1, F. Mozer 2, and D.-H. Lee 1 1 Department of Astronomy.

Voyager 2 Observations of Magnetic Waves due to Interstellar Pickup Ions Colin J. Joyce Charles W. Smith, Phillip A. Isenberg, Nathan A. Schwadron, Neil.

Drift Resonant Interactions of Radiation Belt Electrons with ULF waves. L. G. Ozeke, I. R. Mann, A. Degeling, V. Amalraj, and I. J. Rae University of Alberta.

Oxygen Injection Events observed by Freja Satellite M. Yamauchi 1, L. Eliasson 1, H. Nilsson 1, R. Lundin 1, and O. Norberg 2 1.Swedish Institute of Space.

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.

Intense Poynting flux at very high latitudes during magnetic storms: GITM simulation results Yue Deng 1 Cheng Sheng 1, Manqi Shi 1, Yanshi Huang 2, Cheryl.

1 Two mechanisms of solar-wind proton entry deep into the near-Moon wake revealed by SELENE (KAGUYA) STP seminar August 26, 2009 Masaki N. Nishino* 1 Collaborators:

Simultaneous in-situ observations of the feature of a typical FTE by Cluster and TC1 Zhang Qinghe Liu Ruiyuan Polar Research Institute of China

PARTICLES IN THE MAGNETOSPHERE

Mass Transport: To the Plasma Sheet – and Beyond!

Particle Transport in the Heliosphere: Part 1 Gaetano Zimbardo Universita’ della Calabria, Cosenza, Italy with contributions from S. Perri, P. Pommois,

WG2 Summary Broke into ring current/plasmasphere and radiation-belt subgroups RING CURRENT Identified events for addressing science questions What is the.

17th Cluster workshop Uppsala, Sweden , May 12-15, 2009

Plasma Heating and Particle Acceleration by Turbulence in Solar Flares Siming Liu Stanford University In collaboration with Vahé Petrosian, Yanwei Jiang,

Compressibility and scaling in the solar wind as measured by ACE spacecraft Bogdan A. Hnat Collaborators: Sandra C. Chapman and George Rowlands; University.

H. Hasegawa(1), A. Retinò(2), A. Vaivads(3), Y. Khotyaintsev(3), M

Magnetic reconnection in the magnetotail: Geotail observations T. Nagai Tokyo Institute of Technology World Space Environment Forum 2005 May 4, 2005 Wednesday.

Multi-Spacecraft Observation of Compressional Mode ULF Waves Excitation and Relativistic Electron Acceleration X. Shao 1, L. C. Tan 1, A. S. Sharma 1,

The Geomagnetic Cusps: Magnetic Topology and Physical Processes Antonius Otto Thanks to: Eric Adamson, Katariina Nykyri, Julia Pilchowski, Jason McDonald.

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.

Storm-dependent Radiation Belt Dynamics Mei-Ching Fok NASA Goddard Space Flight Center, USA Richard Horne, Nigel Meredith, Sarah Glauert British Antarctic.

© 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.

SS Special Section of JGR Space Physics Marks Polar’s 5th Anniversary September 4, 1996 This April special section is first of two Polar special sections.

Space Science MO&DA Programs - April Page 1 SS Special Section of JGR Space Physics Marks Polar’s 5th Anniversary September 4, 1996 This April special.

Magnetotail Reconnection T. Nagai Tokyo Institute of Technology Harry Petschek Symposium on Magnetic Reconnection March 22, 2006 Wednesday 12:00 – 12:30.

Richard Thorne / UCLA Physical Processes Responsible for Relativistic Electron Variability in the Outer Radiation Zone over the Solar Cycle 1 Outline 2.

A Global Hybrid Simulation Study of the Solar Wind Interaction with the Moon David Schriver ESS 265 – June 2, 2005.

Source and seed populations for relativistic electrons: Their roles in radiation belt changes A. N. Jaynes1, D. N. Baker1, H. J. Singer2, J. V. Rodriguez3,4.

Modulation of chorus wave intensity by ULF waves from Van Allen Probes Observation Lunjin Chen 1, Zhiyang Xia 1, Lei Dai 2 1 Physics Dept., The University.

Cluster observation of electron acceleration by ULF Alfvén waves

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

ARTEMIS – solar wind/ shocks

Stochastic Acceleration in Turbulence:

Oxygen Injection Events observed by Freja Satellite

D.N. Baker, S. Kanekal, X. Li, S. Elkington

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

Richard B. Horne British Antarctic Survey Cambridge UK

Presentation transcript:

Cusp Radiation Source: A Challenge for Theory and Simulation Jiasheng Chen, Theodore A. Fritz, Katherine E. Whitaker, Forrest S. Mozer, and Robert B. Sheldon In cooperation with: J. F. Fennell, M. Klida, K. Kudela, V. N. Lutsenko, J. Niehof, J. S. Pickett, J. Roeder, C. T. Russell, G. L. Siscoe, W. N. Spjeldvik, and K. Trattner

Theory and simulation predict: Cusp is a precipitation region for particles; A positive IMF By would move the dayside northern cusp into post-noon; A negative IMF By would move the dayside northern cusp into pre-noon (e.g., Cowley et al., JGR, 96, 5557, 1991).

Cusp Diamagnetic Cavities (CDC): |B| CDC at 9:30 MLT (pre-noon) with turbulence. Cusp energetic Particle (CEP)

Cusp CDC at UT on 5/13/99 with a size of ~ 6 Re.

Solar wind conditions for the 5/13/99 CDC Since B y < 0, a CDC at pre-noon was expected. B y < 0

Other CDC observations under different solar wind conditions: 1. Normal solar wind speed, v sw = 450 km/s 2. Fast solar wind stream, v sw = 900 km/s 3. Slow solar wind flow, v sw = 380 km/s (two examples presented)

1. Normal solar wind speed, v sw =450 km/s 4/22/99

(Fritz et al., JGR, 108, A1, 1028, 2003) Pre-noon Post-noon

B y >0, =1.6 nT, CDC at pre-noon; unexpected B y >0 CDC at 10:30 MLT

2. Fast solar wind stream, v sw =900 km/s 6/28/99

Cusp energetic He++ Cusp energetic O+

B y >0, =14.7 nT, CDC at 7MLT; unexpected CDC + +

3a. Slow solar wind flow, v sw =380 km/s 4/25/99

POLAR, 4/25/99

B y >0, =5.5 nT, CDC at pre-noon; unexpected B y >0 CDC at 10:20 MLT

3b. Slow solar wind flow, v sw =380 km/s 15 UT 19 UT 15 UT 19 UT

B y >0, =-82 nT, CDC at 8:30 MLT; unexpected B y >0 CDC 10/30/78 ISEE-1 ISEE-3 IMF

Energetic Charged Particles in CDC CEP electron CEP proton CDC

CEP Energy Spectrum

CEP vs. Outer Radiation Belt Particles Proton phase space density

He++ & O+ phase space densities:  Cusp Radiation Source

CEP and Fields 1.CEP flux increase with E-field increase and B-field Decrease. 2. Emax = 50 mV/m

Blow up cusp E-field near peak fluctuation Showing some polarization Waves at different Frequencies.

Left-hand polarization

Left-hand polarization

Summary CDC is a large radiation region, and CEP is a new radiation source. Under different solar wind and geomagnetic conditions, CDCs have been observed at pre-noon in the northern hemisphere when IMF B y >0 (duskward). These observations are unexpected by the existing models and MHD simulations and provide a new challenge for the current theory and simulations. Cusp ions can be energized by both resonant and stochastic acceleration mechanisms.