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

Slides:

Advertisements

Similar presentations

The challenges and problems in measuring energetic electron precipitation into the atmosphere. Mark A. Clilverd British Antarctic Survey, Cambridge, United.

Advertisements

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.

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.

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.

1 FIREBIRD Science Overview Marcello Ruffolo Nathan Hyatt Jordan Maxwell 2 August 2013FIREBIRD Science.

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.

4/18 6:08 UT 4/17 6:09 UT Average polar cap flux North cap South cap… South cap South enter (need to modify search so we are here) South exit SAA Kress,

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.

Pitch-Angle Scattering of Relativistic Electrons at Earth’s Inner Radiation Belt with EMIC Waves Xi Shao and K. Papadopoulos Department of Astronomy University.

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,

Further development of modeling of spatial distribution of energetic electron fluxes near Europa M. V. Podzolko 1, I. V. Getselev 1, Yu. I. Gubar 1, I.

Monitoring of auroral oval location and geomagnetic activity based on magnetic measurements from satellites in low Earth orbit. S. Vennerstrom Technical.

Modelling the Thermosphere-Ionosphere Response to Space Weather Effects: the Problem with the Inputs Alan Aylward, George Millward, Alex Lotinga Atmospheric.

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

Earth’s Radiation Belt Xi Shao Department of Astronomy, University Of Maryland, College Park, MD

GEM Workshop June 24, 2003 Data Assimilation Workshop Notes Why and What is Data Assimilation? What Data Assimilation is not Key Challenges in Data Assimilation.

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

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,

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

Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results S. A. Ledvina 1, D. Odstrcil 2 and J. G. Luhmann 1 1.Space Sciences.

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

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

Overview of CISM Magnetosphere Research Mary Hudson 1, Anthony Chan 2, Scot Elkington 3, Brian Kress 1, William Lotko 1, Paul Melanson 1, David Murr 1,

New Operational Algorithms for Charged Particle Data from Low-Altitude Polar-Orbiting Satellites J. L. Machol 1,2 *, J.C. Green 1, J.V. Rodriguez 3,4,

Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland

Radiation conditions during the GAMMA-400 observations:

1 Introduction The TOP-modelPotential applicationsConclusion The Transient Observations-based Particle Model and its potential application in radiation.

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.

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

Space Science MO&DA Programs - August Page 1 SS Polar Quantifies Magnetospheric Drivers of Upper Atmospheric Chemistry Changes High resolution global.

Computational Model of Energetic Particle Fluxes in the Magnetosphere Computer Systems Yu (Evans) Xiang Mentor: Dr. John Guillory, George Mason.

The PLANETOCOSMICS Geant4 application L. Desorgher Physikalisches Institut, University of Bern.

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.

Nowcast model of low energy electrons (1-150 keV) for surface charging hazards Natalia Ganushkina Finnish Meteorological Institute, Helsinki, Finland.

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.

1 The Inner Magnetosphere Nathaniel Stickley George Mason University.

Dynamics of the Radiation Belts & the Ring Current Ioannis A. Daglis Institute for Space Applications Athens.

Space Science MO&DA Programs - September Page 1 SS It is known that the aurora is created by intense electron beams which impact the upper atmosphere.

2009 ILWS Workshop, Ubatuba, October 4-9, 2009 Transverse magnetospheric currents and great geomagnetic storms E.E.Antonova (1,2), M. V. Stepanova (3),

SOLAR EXTREME EVENTS AND GRATE GEOMAGNETIC STORMS E.E. Antonova, M.V. Stepanova Skobeltsyn Institute of Nuclear Physics Moscow State University, Moscow,

Data Assimilation With VERB Code

Proposed project on lightning-induced electron precipitation (LEP) Lightning produces VLF waves that propagate globally in the Earth- ionosphere waveguide.

PARTICLES IN THE MAGNETOSPHERE

June 30, 2011 Plasma Pressure Constraints on Magnetic Field Structure in the Substorm Growth Phase Sorin G. Zaharia 1 and Chih-Ping Wang.

1 Space technology course : Space Radiation Environment and its Effects on Spacecraft Components and Systems Space radiation environment Space Radiation.

Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University.

The Geoeffectiveness of Solar Cycle 23 as inferred from a Physics-Based Storm Model LWS Grant NAG Principal Investigator: Vania K. Jordanova Institute.

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

Space Weather in Earth’s magnetosphere MODELS  DATA  TOOLS  SYSTEMS  SERVICES  INNOVATIVE SOLUTIONS Space Weather Researc h Center Masha Kuznetsova.

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,

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

Magnetically Self-Consistent Simulations of Ring Current with Implications for Diffuse Aurora and PIXIE Data Interpretation Margaret W. Chen 1 and Michael.

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.

Energy inputs from Magnetosphere to the Ionosphere/Thermosphere ASP research review Yue Deng April 12 nd, 2007.

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

30 April 2009 Space Weather Workshop 2009 The Challenge of Predicting the Ionosphere: Recent results from CISM. W. Jeffrey Hughes Center for Integrated.

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.

Radiation Belt Storm Probes Mission and the Ionosphere-Thermosphere RPSP SWG Meeting June 2009.

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.

Principal Components of Electron Belt Variation

THEMIS and Space Weather

Thermosphere-Ionosphere Issues for DASI - I:

Extreme Events In The Earth’s Electron Radiation Belts

Geoffrey Reeves LANL.gov NewMexicoConsortium.org

Richard B. Horne British Antarctic Survey Cambridge UK

Magnetosphere: Structure and Properties

Presentation transcript:

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

DREAM: The Dynamic Radiation Environment Assimilation Model Developed by LANL to quantify risks from natural and nuclear belts Uses Kalman Filter, satellite observations, and physics model Couples ring current, magnetic field, and radiation belt models Goals: Specification, Prediction, Understanding

Why Data Assimilation? Complex Physical System Sparse and/or Heterogeneous Observations Global, Real-Time Data-Driven Solution

DREAM Computational Framework

Distribution at L*=6 Observations 1/ /1001/1000 Obsv / Flux vs L*, Time (1 MeV) HEO Observations (validation set) AE-8 Model CRRES-ELE Model DREAM Model DREAM 1/ /1001/1000 Model / CRRES-ELE 1/ /1001/1000 Model / AE-8 1/ /1001/1000

Validation 2: Average Flux vs Altitude

Validation 3: Prediction Efficiency testing variation around the mean PE = 1 - Σ (model - obsv) Σ ( obsv- ) 2 2

Validation 4: Average absolute error DREAM gives ~10x improvement Cumulative Error ( |model – obsv| ) Σ

Connecting DREAM to LEO Precipitating Electron Observations at LEO Trapped Electron Observations This hole is only due to Satellite data coverage LEO observations are critical: auroral, MeV electrons, MeV ions and NPOES instruments (post Nunn-McCurdy) are deficient LEO informs not only the local space weather conditions but also global models of surface charging, internal charging, dose, etc Extrapolating trapped particle models to LEO is challenging LEO observations are critical: auroral, MeV electrons, MeV ions and NPOES instruments (post Nunn-McCurdy) are deficient LEO informs not only the local space weather conditions but also global models of surface charging, internal charging, dose, etc Extrapolating trapped particle models to LEO is challenging POLAR SAMPEX (and LEO to DREAM)

The Opportunities and Challenges of LEO LEO is heavily populated and an important region to predict LEO satellites provide global coverage at high cadence LEO measures ionospheric input But, only a small fraction of particles reach LEO Field asymmetries such as the SSA Time and activity- dependent precipitation α = 10° 20° 30°

POLAR and SAMPEX: 2 MeV electron flux

POLAR and SAMPEX on the same scale

The flux ratio varies from 0.1 to with Time, L, Activity POLAR SAMPEX SAMPEX/POLAR Ratio

POES: Ratio of precipitating/trapped flux can be better understood in physical context keV keV keV Plasmasphere

The RAM-SCB provide further information on coupling of trapped fluxes to LEO & the ionosphere Perpendicular PressureAzimuthal Current Density

RAM-SCB calculates EMIC & Whistler wave growth, amplitude, & wave-particle interactions EMIC Wave Gain Plasmaspheric Electron Density EMIC Wave Amplitude

Precipitating 1 MeV electron and 100 keV ion fluxes as a function of L, LT, and time

RAM-SCB and the SW Modeling Framework 1-way coupling has been demonstrated 2-way is in development

Realistic calculation of ring current is the first step for calculation of Region 2 currents BATSRUS ~ zero Dst RAM-SCB - stronger RC than SWMF (BATSRUS+RCM) Including O+ implies fewer ions and weaker Dst E-field very strong in recovery phase– will change with shielding Tail current (> 6.6 R E ) not included (~ 30% of Dst?)

RAM-SCB equatorial B field is much lower and has more structure than SWMF SWMF RAM-SCB Artifacts at L<3.5 are due to imperfect model grid matching

Realistic calculation of ring current pressures and B produce very realistic R2 currents 3D equilibrium code calculates currents from pressure gradients and force- balanced B-field much sharper resolution (field line inter-distance increases toward Earth) SWMF – R-1 currents; very small R-2 currents no shielding RAM-SCB: R-2 currents at lower latitudes; some R-1 currents higher

DREAM at LEO : Conclusions Extrapolating global radiation belt models to LEO is complex Assimilating LEO fluxes into a global model could produce large (>10 3 ) errors if not done properly “Properly” means considering dependence on energy, local time, geomagnetic activity, magnetospheric regions… Local pitch angle information hugely helps understand different behavior in trapped, bounce-loss, & drift-loss cones LEO measurements (if any) help more than just LEO satellites