Interaction of Shear Alfven Waves (SAW) with Trapped Energetic Protons in the Inner Radiation Belt X. Shao, K. Papadopoulos, A. S. Sharma Department of.

Slides:



Advertisements
Similar presentations
RFQ Cooling Studies.
Advertisements

Introduction to Plasma-Surface Interactions Lecture 6 Divertors.
Limiting Energy Spectrum of a Saturated Radiation Belt Michael Schulz 1037 Twin Oak Court Redwood City, CA (USA) from Schulz and Davidson [JGR, 93,
Jacob Bortnik 1,2, PhD 1 Department of Atmospheric & Oceanic Sciences, University of California at Los Angeles, CA 2 Visiting Scholar, Center for Solar-Terrestrial.
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.
Influence of EMIC Waves on Radiation Belt Dynamics T. Kersten, R. B. Horne, N. P. Meredith, S. A. Glauert ESWW11 Liège, 17-21/11/2014 British Antarctic.
1 FIREBIRD Science Overview Marcello Ruffolo Nathan Hyatt Jordan Maxwell 2 August 2013FIREBIRD Science.
The Importance of Wave Acceleration and Loss for Dynamic Radiation Belt Models Richard B. Horne M. M. Lam, N. P. Meredith and S. A. Glauert, British Antarctic.
Electron Acceleration inside Jupiter’s Radiation Belt and the Origin of Synchrotron Radiation Richard B. Horne 1 R. M. Thorne 2, S. A. Glauert 1, J. D.
Pitch-Angle Scattering of Relativistic Electrons at Earth’s Inner Radiation Belt with EMIC Waves Xi Shao and K. Papadopoulos Department of Astronomy University.
Single particle motion and trapped particles
21 ECRS, Kosice, 12/09/2008 Trapped charge particles measurements in the radiation belt by PAMELA instrument Vladimir V. Mikhailov (MEPHI) for PAMELA collaboration.
INTRODUCTION OF WAVE-PARTICLE RESONANCE IN TOKAMAKS J.Q. Dong Southwestern Institute of Physics Chengdu, China International School on Plasma Turbulence.
Dennis Papadopoulos University of Maryland, College Park .
DISTRIBUTION D: Distribution authorized to Department of Defense and DoD contractors (Administrative or Operational Use); 10 Dec Other requests for.
Modeling Generation and Nonlinear Evolution of Plasma Turbulence for Radiation Belt Remediation Center for Space Science & Engineering Research Virginia.
Earth’s Radiation Belt Xi Shao Department of Astronomy, University Of Maryland, College Park, MD
Physics of fusion power Lecture 11: Diagnostics / heating.
HF Focusing due to Field Aligned Density Perturbations A. Vartanyan 1, G. M. Milikh 1, K. Papadopoulos 1, M. Parrot 2 1 Departments of Physics and Astronomy,
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,
Stanford Wave Induced Particle Precipitation (WIPP) Code Prajwal Kulkarni U.S. Inan, T.F. Bell March 4, 2008 Space, Telecommunications and Radioscience.
Physics of fusion power Lecture 14: Collisions / Transport.
Finite Temperature Effects on VLF-Induced Precipitation Praj Kulkarni, U.S. Inan and T. F. Bell MURI Review February 18, 2009.
Spectral analysis of non-thermal filaments in Cas A Miguel Araya D. Lomiashvili, C. Chang, M. Lyutikov, W. Cui Department of Physics, Purdue University.
Global Distribution / Structure of Aurora Photograph by Jan Curtis Synthetic Aurora pre- midnight,multi-banded Resonant ULF waves produce pre- midnight,
Magnetospheric Morphology Prepared by Prajwal Kulkarni and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global.
Nonresonant pitch angle scattering of electrons and breakdown of adiabatic invariance: Modeling Surja Sharma, Alexey Karavaev, Erin Lynch, Nail Gumerov,
Physics of fusion power
Wave-Particle Interaction
Kinetic Effects in the Magnetosphere Richard E Denton Dartmouth College.
RESONANCE Project for Studies of Wave-Particle Interactions in the Inner Magnetosphere Anatoly Petrukovich and Resonance team RESONANCEРЕЗОНАНС R.
ELECTRON ACCELERATION BY TIME DOMAIN STRUCTURES (TDS) by Mozer, F.S., O.V. Agapitov, A.V. Artemyev, V. Krasnoselskikh, and I. Vasko OUTLINE 1.Experimental.
Nonlinear VLF Wave Physics in the Radiation Belts Chris Crabtree Guru Ganguli Erik Tejero Naval Research Laboratory Leonid Rudakov Icarus Research Inc.
D. Sibeck, R. Millan, H. Spence
Does Fermi Acceleration of account for variations of the fluxes of radiation belt particles observations at low altitudes during geomagnetic storms? J.
Comparisons of Inner Radiation Belt Formation in Planetary Magnetospheres Richard B Horne British Antarctic Survey Cambridge Invited.
HAGIS Code Lynton Appel … on behalf of Simon Pinches and the HAGIS users CCFE is the fusion research arm of the United Kingdom Atomic Energy Authority.
ASEN 5335 Aerospace Environments -- Radiation Belts1 The Radiation Belts A radiation belt is a population of energetic particles stably-trapped by the.
L ONG - TERM VERB CODE SIMULATIONS OF ULTRA - RELATIVISTIC ELECTIONS AND COMPARISON WITH V AN A LLEN P ROBES MEASUREMENTS Drozdov A. Y. 1,2, Shprits Y.
Outline > does the presence of NL waves affect the conclusion that QL acceleration suffices? > it depends... Outline Large amplitude whistler waves Limitations.
1 The Inner Magnetosphere Nathaniel Stickley George Mason University.
Travelling Wave Tube For Broadband amplifier helix TWTs (proposed by Pierce and others in 1946 ) are widely used For High average power purposes the.
Radiation belt particle dynamics Prepared by Kevin Graf Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global AWESOME Network.
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.
Observation of global electromagnetic resonances by low-orbiting satellites Surkov V. V. National Research Nuclear University MEPhI.
Coupling of the Magnetosphere and Ionosphere by Alfvén Waves at High and Mid-Latitudes Bob Lysak, Yan Song, University of Minnesota, MN, USA Murray Sciffer,
Outline Motivation and observation The wave code solves a collisional Hall-MHD model based on Faraday’s and Ampere’s laws respectively, coupled with.
Whistler Waves and Related Magnetospheric Phenomena
Proposed project on lightning-induced electron precipitation (LEP) Lightning produces VLF waves that propagate globally in the Earth- ionosphere waveguide.
Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University.
Multi-Spacecraft Observation of Compressional Mode ULF Waves Excitation and Relativistic Electron Acceleration X. Shao 1, L. C. Tan 1, A. S. Sharma 1,
Storm-dependent Radiation Belt Dynamics Mei-Ching Fok NASA Goddard Space Flight Center, USA Richard Horne, Nigel Meredith, Sarah Glauert British Antarctic.
SuperDARN:Looking ahead to RBSP Jim Wild Physics Department, Lancaster University, UK Tim Yeoman & Robert Fear Department of Physics & Astronomy, University.
Lecture 15 Modeling the Inner Magnetosphere. The Inner Magnetosphere The inner magnetosphere includes the ring current made up of electrons and ions in.
The Role of VLF Transmitters in Limiting the Earthward Penetration of Ultra-Relativistic Electrons in the Radiation Belts J. C. Foster, D. N. Baker, P.J.
Modelling Electron Radiation Belt Variations During Geomagnetic Storms with the new BAS Global Radiation Belt Model Richard B. Horne Sarah A. Glauert Nigel.
–11.03 Hawaii Multi bunch acceleration on LUCX system Ⅰ. LUCX project Ⅱ. Simulation results for Compton scattering Ⅲ. Calculation on beam loading.
Evolution of the poloidal Alfven waves in 3D dipole geometry Jiwon Choi and Dong-Hun Lee School of Space Research, Kyung Hee University 5 th East-Asia.
AGILE as particle monitor: an update
Plasma Wave Excitation Regions in the Earth’s Global Magnetosphere
VNC: Application of Physics and Systems Science methodologies to Forecasting of the Radiation Belt Electron Environment S. N. Walker1, M. A. Balikhin1,
ESS 154/200C Lecture 15 The Inner Magnetosphere II
Definitive Mapping in the Late Growth Phase
Single particle motion and trapped particles
Ch32: Electromagnetic Waves
Collaborators: Xin Tao, Richard M. Thorne
ICRC2003 OG Calculation of Cosmic-Ray Proton and Anti-proton Spatial Distribution in Magnetosphere Michio Fuki, Ayako Kuwahara, Nozomi, Sawada Faculty.
Electromagnetic Waves
Richard B. Horne British Antarctic Survey Cambridge UK
Magnetosphere: Structure and Properties
Presentation transcript:

Interaction of Shear Alfven Waves (SAW) with Trapped Energetic Protons in the Inner Radiation Belt X. Shao, K. Papadopoulos, A. S. Sharma Department of Physics and Astronomy, University of Maryland, College Park, MD, USA

Outline Proton-SAW Gyro-Resonant Condition Frequency selection for SAW-Proton resonance under inner belt condition Proton lifetime as a function of average SAW amplitude Ground-injected SAW power as a function of energy stored per unit shell volume

Proton-SAW Gyro-Resonant Condition Gyro-Resonant Condition: (non-relativistic proton, ω << Ω) SAW Dispersion Relation: Gyro-Resonant Condition for proton (v, ) with SAW:

Frequency Selection for Proton-SAW Resonance Proton Energy Frequency Range 30 MeV6-16 Hz 50 MeV5-15 Hz 100 MeV Hz Frequency requirement for equatorial Proton-SAW resonance with at L=1.5 Frequency range ~ 5-15 Hz Broadband SAW:

Proton Lifetime Calculation I 1. Local Pitch Angle Diffusion Rate Proportional to Wave Energy 2. Bounce Averaged Diffusion Rate λ is the latitude and φ is the azimuthal angle (Wave energy trapped inside flux tube at φ)

Proton Lifetime Calculation II 3.Drift-Averaged Pitch Angle Diffusion Rate Pitch angle scattering amount is proportional to the stored SAW energy the proton experiences during its bounce-drift orbit.

Proton Lifetime Calculation III (Life Time) 4. Solve Pitch-Angle Diffusion Equation Use finite-difference to discretize Use iterative method to solve nonlinear eigen-value problem for lifetime Split temporal and pitch angle distribution

Local PAD Rate L = 1.5 for 30 MeV protons in presence of waves with f 0 = 13 Hz, Δf = 0.5 f 0 δB = 25 pT, (10 8 sec ~ 3 years) Alfven Velocity along L = 1.5 Field line From Global Core Plasma Model + Dipole Model Shift is due to increase of B Local Pitch-Angle Diffusion (PAD) Rate for Protons at L = 1.5 Loss Cone Earth Equator

Drift-Bounce Averaged PAD Rate  f/f=1/2, = 25 pT 6.5 Hz10 Hz 13 Hz Energy stored in SAW at L=1.5 and DL=.1 (volume = 3 x m^3) with =25 pT is W= 75 kJ Loss Cone

Proton Lifetime f 1 = 6.5 Hzf 2 = 10 Hzf 3 = 13 Hz E = 30 MeV1688 days880 days595 days E = 50 MeV900 days586 days920 days E = 100 MeV580 days1032 days1600 days Df/f=1/2, Energy stored in SAW at L=1.5 and DL=.1 is W= 75 kJ Life time of ( MeV) protons can be reduced to 1-3 years.

Injection of SAW Ionospheric Reflection Injection can be carried out at selected sites The remediation effects will be the same for global or sector injection as long as the total stored SAW resonance energy is the same. SAW is trapped inside the flux tube The loss of SAW mainly occurs at the ionospheric boundary.

Injection Power Requirement Injection power required to maintain 75 kJ at L=1.5 per.1 L width Typically, the required SAW injection power is ~ kW to reduce life time of ( MeV) protons to 1-3 years. Wave Energy Evolution in Leaky Cavity R: Ionospheric Reflection Coefficient ΔT: Alfven Wave Travel Time R=

Summary Estimates indicate that less than kWatt level of ULF injected into the L = region is required to get interesting PRB removal lifetime (1-3 years).