U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Direct measurements of chorus wave effects on electrons in the.

Slides:

Advertisements

Similar presentations

Improving Salammbô model and coupling it with IMPTAM model V. Maget 1 D. Boscher 1, A. Sicard-Piet 1, N. Ganushkina 2 1. ONERA, Toulouse, FRANCE 2. FMI,

Advertisements

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

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.

Operated by Los Alamos National Security, LLC for the U.S. Department of Energy’s NNSA U N C L A S S I F I E D A Detailed Look at Energetic Electron Dynamics.

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.

Forecasting the high-energy electron flux throughout the radiation belts Sarah Glauert British Antarctic Survey, Cambridge, UK SPACECAST stakeholders meeting,

U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Pitch angle evolution of energetic electrons at geosynchronous.

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.

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.

U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Once Upon a Time in the Electron Radiation Belts R. Friedel,

Radiation Belt Electron Pitch Angle Measurements from the GOES Satellites T. G. Onsager, J. C. Green, and H. J. Singer NOAA Geostationary Operational Environmental.

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.

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 and interplanetary origin of geomagnetic storms Sources, acceleration, and losses of ring current ions Modeling the evolution of the terrestrial.

1 TOWARD PREDICTING VLF TRIGGERING MURI Workshop 3 March 2008 E. Mishin and A. Gibby Boston College ISR Stanford University STAR Lab.

Storm-Time Dynamics of the Inner Magnetosphere: Observations of Sources and Transport Michelle F. Thomsen Los Alamos National Laboratory 27 June 2003.

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

Finite Temperature Effects on VLF-Induced Precipitation Praj Kulkarni, U.S. Inan and T. F. Bell MURI Review February 18, 2009.

Magnetospheric Morphology Prepared by Prajwal Kulkarni and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global.

Motivation + Objective  Previous statistical results are limited due to frequency coverage (> 100 Hz) and lack of polarization properties.  Unusually.

UCLA-LANL Reanalysis Project Yuri Shprits 1 Collaborators: Binbin Ni 1, Dmitri Kondrashov 1, Yue Chen 2, Josef Koller 2,

RBSP-ECT Suite Status: Instrument Status and Instrument Operations Flexibility Harlan E. Spence on behalf of RBSP-ECT Team University of New Hampshire.

Van Allen Probes, NOAA, and Ground Observations of a Pc 1 Wave Event Extending 12 Hours in MLT Mark Engebretson 1, Jennifer Posch 1, John Wygant 2, Craig.

Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland

Nonlinear VLF Wave Physics in the Radiation Belts Chris Crabtree Guru Ganguli Erik Tejero Naval Research Laboratory Leonid Rudakov Icarus Research Inc.

Comparisons of Inner Radiation Belt Formation in Planetary Magnetospheres Richard B Horne British Antarctic Survey Cambridge Invited.

Understanding and Mitigating Radiation Belt Hazards for Space Exploration Geoffrey Reeves Space Science and Applications, ISR-1, Los Alamos National Laboratory,

First Direct Experimental Measurement of loss cone scattering of energetic electrons by whistler mode hiss in the plasmasphere Van Allen Probes/BARREL.

RBSP SWG Meeting 1 3/5/2009 BARREL Update (Balloon Array for RBSP Relativistic Electron Losses) R. M. Millan and the BARREL Team.

Hot He + events in the inner magnetosphere observed by Cluster M. Yamauchi 1, I. Dandouras 2, H. Reme 2, H. Nilsson 1 (1) Swedish Institute of Space Physics.

ORBITALS Phase A Extended Interim Meeting U of A Phase A2 Work Update ORBITALS Science Team, University of Alberta CSA HQ, St. Hubert, 2010/03/17.

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.

U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA The Role of Cold Plasma Density in Radiation belt Dynamics R.

A statistical study of the Field-Aligned Electron Events (status report) Solène Lejosne, Forrest Mozer and Oleksiy Agapitov SSL, University of California,

PAPER I. ENA DATA ANALYSIS RESULTS. The Imager for Magnetopause-to- Aurora Global Exploration (IMAGE) missionis the first NASA Mid-size Explorer (MIDEX)

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.

Kinetic-scale electric field structures at plasma boundaries in the inner magnetosphere (including injection fronts) David Malaspina 1, John Wygant 2,

U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Wave particle Interactions in the Inner Magnetosphere R. Friedel.

Plasma Density Structures in the Inner Magnetosphere Derived From RPI Measurements B. Reinisch 1, X. Huang 1, P. Song 1, J. Green 2, S. Fung 2 V. Vasyliunas.

Plasmasphere Refilling Rates Inferred from Polar and IMAGE Satellite Spectrogram Data T. Huegerich(1), J. Goldstein(1), P.H. Reiff(1), B.W. Reinisch(2)

Effective drift velocity and initiation times of interplanetary type-III radio bursts Dennis K. Haggerty and Edmond C. Roelof The Johns Hopkins University.

Scott Thaller Van Allen Probes EFW meeting University of Minnesota June 10-12, 2014.

Low-Altitude Mapping of Ring Current and Radiation Belt Results Geoff Reeves, Yue Chen, Vania Jordanova, Sorin Zaharia, Mike Henderson, and Dan Welling.

Multi-point observations of dispersionless injection fronts inside geostationary orbit: propagation and structure Authors (preliminary) David Malaspina.

Dynamic features of plasmapause revealed by in situ measurements from Van Allen and THEMIS Probes Sam Califf et al.

Hot He + events in the inner magnetosphere observed by Cluster 1 Yamauchi, et al. (2014), JGR, doi: /2013JA Inner magnetosphere: Majority.

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

Slide 1 Operated by Los Alamos National Security, LLC for the U.S. Department of Energy's NNSA UNCLASSIFIED The Global Positioning System as a Space Weather.

Nonlinear electric field structures in the inner magnetosphere D. M. Malaspina 1, L. Andersson 1, R. E. Ergun 1, J. R. Wygant 2, J. W. Bonnell 3, C. Kletzing.

The large scale convection electric field, ring current energization, and plasmasphere erosion in the June 1, 2013 storm Scott Thaller Van Allen Probes.

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

Dual S/C observations of shock-driven electron acceleration AB Y GSM (R E ) X GSM (R E ) Lstar.

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

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.

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.

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,

M. Yamauchi1, I. Dandouras2, H. Reme2,

R. Bucˇık , K. Kudela and S. N. Kuznetsov

Yuki Takagi1*, Kazuo Shiokawa1, Yuichi Otsuka1, and Martin Connors2

Ulysses COSPIN High Energy Telescope observations of cosmic ray and solar energetic particles intensities since its distant Jupiter flyby in 2004 R.B.

Yue Chen (Los Alamos National Laboratory)

Collaborators: Xin Tao, Richard M. Thorne

Geoffrey Reeves LANL.gov NewMexicoConsortium.org

Statistical analysis of hiss wave spectrum from the EMFISIS wave data

Richard B. Horne British Antarctic Survey Cambridge UK

Presentation transcript:

U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Direct measurements of chorus wave effects on electrons in the 5-40 KeV range from the Van Allen Probes Mission R. Friedel 1, Z. Hong 2, B. Larsen 1, G. Reeves 1, R. Skoug 1, C. Kletzing 3, M. Henderson 1 and Y. Chen 1 LANL 1, LASP 2,University of Iowa 3

U N C L A S S I F I E D Slide 2 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Contents Motivation Pitch angle Statistics from HOPE and MagEIS – Pitch angle model – First results Two Spacecraft Event Selection – Matching Drift Paths – Filtering ephemeris information Event with waves at spacecraft at later MLT Event with NO waves Events summary Summary/Conclusion

U N C L A S S I F I E D Slide 3 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Motivation The Van Allen Probe Mission with 2 spacecraft and exquisite particle and wave instrumentation is designed to explore the effects of Magnetospheric waves on the in-situ particle populations. We focus on the region of most active chorus wave activity, just outside the plasmapause, and on the energy range of particles most strongly affected by chorus waves (10's of keV, the top energy range of HOPE), and seek out changes in the pitch angle distribution (PAD) of the electrons that drift from one probe to the other– in either the presence or absence of chorus waves. Hypothesis: – We expect NO change in the PAD or flux levels for NO waves. – We expect a lowering of the flux levels and a flattening of the PAD (isotropization) in the presence of waves.

U N C L A S S I F I E D Slide 4 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Pitch angle distribution (PAD) characterization / fitting (Chen et al., 2014) Use Legendre polynomials – where α is the pitch angle, j is the flux, P n is the Legendre polynomial, C n is the corresponding coefficient. – P 0, P 2, P 4, P 6 …: symmetric; P 1, P 3, P 5, ….: asymmetric Normalization – Directionally averaged flux Only keep c 2, c 4 and c 6 for statistics PAD Selection – Equatorial PAD – counts >50 – assume 90 O symmetry – keep good fits only

U N C L A S S I F I E D Slide 5 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Pitch angle distribution (PAD) characterization / fitting (Chen et al., 2014) Butterfly PAD: negative c4 Normal PAD Butterfly PAD Flattop PAD

U N C L A S S I F I E D Slide 6 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 PAD comparison under different Kp (MagEIS E=35 keV) c4 c6 c2 Kp > 3+1+ < Kp ≤ 3+Kp ≤ 1+ Work done by Z. Hong, 2014 LANL SW Summer School

U N C L A S S I F I E D Slide 7 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 L=4.0 L=4.8L=5.5 PAD comparison under different Kp (MagEIS E=35 keV) – Sample PADs Inside Plasmasphere -> Outside Plasmasphere 90 O -> “Head and Shoulders” Work done by Z. Hong, 2014 LANL SW Summer School

U N C L A S S I F I E D Slide 8 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 PAD comparison under different Kp (HOPE E=5 keV) c4 c6 c2 Kp > 3+1+ < Kp ≤ 3+Kp ≤ 1+ Work done by Z. Hong, 2014 LANL SW Summer School

U N C L A S S I F I E D Slide 9 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 PAD comparison under different Kp (HOPE E=5 keV) – Sample PADs Inside Plasmasphere -> Outside Plasmasphere 90 O -> Very weak “Head and Shoulders” L=4.0 L=5.0 L=5.8 Work done by Z. Hong, 2014 LANL SW Summer School Kp ≤ 1+

U N C L A S S I F I E D Slide 10 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 PAD comparison under different Kp (HOPE E=5 keV) – Sample PADs Inside Plasmasphere -> Outside Plasmasphere 90 O -> Weak “Head and Shoulders” L=4.0 L=5.0 L=5.8 Work done by Z. Hong, 2014 LANL SW Summer School 1+ < Kp ≤ 3+

U N C L A S S I F I E D Slide 11 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 PAD comparison under different Kp (HOPE E=5 keV) – Sample PADs Not enough statistics! L=4.0 L=5.0 L=5.8 Work done by Z. Hong, 2014 LANL SW Summer School Kp > 3+

U N C L A S S I F I E D Slide 12 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Two Spacecraft Event Selection – Criteria Statistical Chorus Occurrence Starts before midnight towards dawn, outside Plasmasphere. Compare RBSP Spacecraft at 0-2 MLT and MLT, when both are near L= Drift paths for electrons 5-40 KeV approximate circular in this sector. Drift times for 4hrs MLT: 35 keV ~ 1 hour 5 keV ~ 10 hours (max radial deviation 0.25 Re) UBK, Dipole / Volland-Stern, KP=3 Mededith, Ae = KeV 5 KeV

U N C L A S S I F I E D Slide 13 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Two Spacecraft Event Selection – Very few events Used first year of HOPE pitch angle data – launch to 09/23/2013 (there is a reason…) A at later MLT wrt to B: :42 to : :40 to : :44 to : :42 to :25 4 B at later MLT wrt to B: :05 to : :02 to : :58 to : :10 to : :11 to :45 5 SUN

U N C L A S S I F I E D Slide 14 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Chorus at A, no chorus at B :10 to 12:41 Pitch angle distribution peaked at 90 at B at 9E6 reduced to 3.7E6 at A ~ 41 % loss RBSP B 5.2keV RBSP A 5.2keV

U N C L A S S I F I E D Slide 15 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 LEO particle precipitation proxy for high altitude wave distribution and intensity (Y. Chen, LANL) Comparing CRRES wave statistics with NOAA 30 KeV precipitation statistics – deriving model relationship

U N C L A S S I F I E D Slide 16 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Proxy for waves for 6hr period centered around :30UT v. “best guess”

U N C L A S S I F I E D Slide 17 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 No chorus at A, no chorus at B :14 to 06:51 Pitch angle distribution peaked at 90 at B at 9E6 reduced to 3.7E6 at A ~ 59% loss RBSP B 5.2keV RBSP A 5.2keV

U N C L A S S I F I E D Slide 18 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Proxy for waves for 6hr period centered around :30UT

U N C L A S S I F I E D Slide 19 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Two Spacecraft Event Summary A or B at 0-2 MLT, L=4.5-5, 5 keV electrons A at later MLT wrt to B: :42 to 10:14 – B in Plasmasphere / structured hiss; A in Plasmasheet boundary :40 to 13:11 – Both outside Plasmasphere, No chorus at B, chorus at A, 59% reduction :44 to 07:21 – Both outside Plasmasphere, No chorus at both, same flux :42 to 10:25 – Both in Plasmasphere, close to plasmapause B at later MLT wrt to B: :05 to 11:38 – Both outside Plasmasphere, No chorus at A, chorus at B, 75% reduction No LEO NOAA data :02 to 08:49 – Both in Plasmasphere, B sees broadband Hiss, A observes no hiss :58 to 11:49 – A in Plasmasheet, with chorus; B in Plasmasphere, hiss :10 to 05:45 – A in Plasmasphere / structured hiss; B in Plasmasheet, no chorus :11 to 08:45 – A in Plasmasphere / curious hiss?; B in Plasmasheet, no chorus

U N C L A S S I F I E D Slide 20 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Study Bonus – Curious Hiss observation Hiss rising tone 2 -4 KHz ~4 min repetition

U N C L A S S I F I E D Slide 21 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Summary / Conclusion Statistical Study: 35 keV: Statistically little variation with Kp. Outside plasmasphere persistent “head and shoulder” distributions – evidence for enhanced PA diffusion at more field-aligned pitch angles. Little variation with MLT 5 keV: Statistically very little variation with Kp. Little variation with MLT, mainly 90 o peaked distributions – surprising given the long drift times and local time distribution of waves. HOPE data still incomplete for coverage at all MLT (noon time sector not covered).

U N C L A S S I F I E D Slide 22 Operated by the Los Alamos National Security, LLC for the DOE/NNSA AGU Chapman Conference, Jeju, South Korea, August 31 – September 5, 2104 Summary / Conclusion Drift – matching case studies: Show measureable depletion of 5 keV electrons in the presence of waves. Very little change in pitch angle distribution shape – what is maintaining anisotropy? No evidence of development of “head and shoulders” distribution as seen in statistics. Study offers opportunity to quantitatively test predictions of wave-particle interaction theory. Future extension of work to use more sophisticated drift matching calculations and extend work to larger energy range.