Stanford Wave Induced Particle Precipitation (WIPP) Code Prajwal Kulkarni U.S. Inan, T.F. Bell March 4, 2008 Space, Telecommunications and Radioscience.

Slides:

Advertisements

Similar presentations

Limiting Energy Spectrum of a Saturated Radiation Belt Michael Schulz 1037 Twin Oak Court Redwood City, CA (USA) from Schulz and Davidson [JGR, 93,

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.

Satellite and Ground Observations of Chorus Emissions Prepared by Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through.

Waves and Particles in the Radiation Belt Kaiti Wang PSSC/NCKU March 17, 2009 Opportunity for Collaboration on ERG and SCOPE Missions & Community Input.

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 Two questions still of the day: the Gendrin angle, the R.Gendrin view on the positioning of URSI F. Lefeuvre LPCE / CNRS – Univ Orléans.

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,

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.

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.

ALTITUDE PROFILES OF ELECTRON DENSITY DURING LEP EVENTS FROM VLF MONITORING OF THE LOWER IONOSPHERE Desanka Šulić 1 and Vladimir Srećković 2 1 Institute.

Modeling Generation and Nonlinear Evolution of VLF Waves for Space Applications W.A. Scales Center of Space Science and Engineering Research Virginia Tech.

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.

Nonlinear Evolution of Whistler Turbulence W.A. Scales, J.J. Wang, and O. Chang Center of Space Science and Engineering Research Virginia Tech L. Rudakov,

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

Subionospheric VLF propagation

Solar Flare Particle Heating via low-beta Reconnection Dietmar Krauss-Varban & Brian T. Welsch Space Sciences Laboratory UC Berkeley Reconnection Workshop.

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

Seasonal dependence of LEP observed on DEMETER Erin S. Gemelos 1, Umran S. Inan 1, Martin Walt 1, Jean-Andre Sauvaud 2, Michel Parrot 3 February 18, 2009.

Damping of Whistler Waves through Mode Conversion to Lower Hybrid Waves in the Ionosphere X. Shao, Bengt Eliasson, A. S. Sharma, K. Papadopoulos, G. Milikh.

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

Targeted VLF Wave-injection Experiments Mark Gołkowski MURI Review Stanford University February 18, 2009.

1 Sounds of VLF Prepared by Morris Cohen and Nader Moussa Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global AWESOME Network.

Dipole antenna: Experiment/theory status Timothy W. Chevalier Umran S. Inan Timothy F. Bell February 18, 2009.

Wave Injection at Low Latitudes Mark Golkowski Remediation of Enhanced Radiation Belts Workshop Lake Arrowhead, CA March 3-6, 2007.

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.

Solar Activity and VLF Prepared by Sheila Bijoor and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global AWESOME.

Whistlers, Magnetospheric Reflections, and Ducts Prepared by Dan Golden, Denys Piddyachiy, and Naoshin Haque Stanford University, Stanford, CA IHY Workshop.

Wave-Particle Interaction

Kinetic Effects in the Magnetosphere Richard E Denton Dartmouth College.

SC-A CIR Event 1 March 2013 CME Event 17 March 2013 SC-A SC-B Enhancement of Inner Zone Electron Fluxes Both events caused electron enhancements for

RESONANCE Project for Studies of Wave-Particle Interactions in the Inner Magnetosphere Anatoly Petrukovich and Resonance team RESONANCEРЕЗОНАНС R.

Ionospheric-magnetospheric VLF Wave Propagation: RPI/IMAGE-HAARP Correlative Study RPI/IMAGE-HAARP Correlative Study V. Paznukhov, B. Reinisch, G. Sales,

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

Solar cycle dependence of EMIC wave frequencies Marc Lessard, Carol Weaver, Erik LindgrenMark Engebretson University of New HampshireAugsburg College Introduction.

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.

© 2008 The Aerospace Corporation Workshop on Coupling of Thunderstorms and Lightning to Near-Earth Space University of Corsica, June 2008 SAMPEX.

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.

Outline > does the presence of NL waves affect the conclusion that QL acceleration suffices? > it depends... Outline Large amplitude whistler waves Limitations.

Rory J Gamble1, Craig J Rodger1, Mark A Clilverd2,

Radiation belt particle dynamics Prepared by Kevin Graf Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global AWESOME Network.

Solar cycle dependence of EMIC wave frequencies Marc Lessard, Carol Weaver, Erik Lindgren 1 Mark Engebretson University of New HampshireAugsburg College.

XVII CLUSTER Workshop, Uppsala, 14 May 2009 Fan and horseshoe instabilities -relation to the low frequency waves registered by Cluster in the polar cusp.

Whistler Waves and Related Magnetospheric Phenomena

IDEE, The Electron Spectrometer for the Taranis Mission J.-A. Sauvaud 1, P. Devoto, A. Fedorov 1, G. Orttner 1, O. Chasselat 1, K. Wong 1, L. Prech 2,

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

2014 LWS/HINODE/IRIS Workshop, Portland OR, Nov 2-6, 2014

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

Van Allen Probes Extended Mission Science Themes (1 of 3) 1.Spatial and temporal structures of injections and other transient phenomena and their effects.

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

Local Acceleration and Loss of Relativistic Electrons in the Earth’s Outer Radiation Belt GEM Workshop Zermatt Resort, Utah 22 nd – 27 th June, 2008 Nigel.

Ground-based transmitter signals observed from space: ducted or nonducted? Craig J. Rodger Department of Physics University of Otago Dunedin NEW ZEALAND.

Nonlinear plasma-wave interactions in ion cyclotron range of frequency N Xiang, C. Y Gan, J. L. Chen, D. Zhou Institute of plasma phsycis, CAS, Hefei J.

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.

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.

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,

The Magnetosphere Feifei Jiang, UCLA

Magnetospheric waves Lauren Blum.

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

Collaborators: Xin Tao, Richard M. Thorne

Geoffrey Reeves LANL.gov NewMexicoConsortium.org

Richard B. Horne British Antarctic Survey Cambridge UK

Presentation transcript:

Stanford Wave Induced Particle Precipitation (WIPP) Code Prajwal Kulkarni U.S. Inan, T.F. Bell March 4, 2008 Space, Telecommunications and Radioscience (STAR) Laboratory Stanford University Stanford, CA

2 Outline 1.Motivation 2.Ground-based VLF Transmitters 3.Wave-Particle Interaction 4.Simulation Results 5.Conclusions

3 Motivation and Procedure  Resonant interactions with waves are responsible for the acceleration and loss of radiation belt electrons.  In the inner belt and slot region, different types of waves (whistlers, hiss, VLF transmitters) are important drivers of precipitation.  Abel and Thorne [1998a]  Inan et al. [1984] used a test particle approach to calculate precipitation zones around existing ground-based VLF transmitters  Considered only ducted propagation  We calculate the precipitation signatures induced by the NPM, NWC, NLK, NAU and NAA ground-based VLF transmitters as well as by hypothetical transmitters  Utilize the Stanford 2D VLF Raytracing program  Calculate Landau damping along raypath [Bell et al., 2002].  Calculate energetic electron precipitation based on method of Bortnik et al. [2005a, 2005b].  We focus on > 100 keV electrons

4 Transmitter Parameters L = 2.75 f = 24.8 kHz 192 kW L = 1.15 f = 21.4 kHz 424 kW L = 2.98 f = 24.0 kHz 1000 kW L = 1.38 f = 19.8 kHz 1000 kW L = 1.30 f = kHz 100 kW

kHz 424 kW L = ° VLF Transmitters

6 No Magnetospheric Reflections  Wave frequency must be below the local lower hybrid resonance frequency, f LHR  f LHR generally below 13 kHz in inner magnetosphere  Increases at locations closer to the surface of the earth.  Ground based transmitters radiate frequencies above the f LHR and therefore do not MR

7 Wave-Particle Interaction  H effectively determines electron resonant velocity Higher frequency waves resonate with lower energy electrons So which factor is most important: location, frequency, radiated power?  H : gyrofrequency  : wave frequency k z : wave k-vector  : relativistic gamma-factor v z : resonant electron velocity

8 Case Study NAA: L = 2.98 (54.6 o ), kHz, 1 MW NAU: L = 1.30 (28.6 o ), kHz, 100 kW Both at 100 kW, NAA location, equatorial interactions Actual locations, 100 kW Off-equatorial interactions Actual characteristics Both at 100 kW Equatorial Interactions

9

10 Role of Source Location

11 Role of Source Location: 100 keV All transmitters at 1 MW radiated power

12 Role of Source Location: 1 MeV All transmitters at 1 MW radiated power

13 Role of Radiated Power

14 Underlying Models

15 Conclusion  We have calculated > 100 keV energetic electron precipitation signatures that would be induced by five existing ground-based VLF transmitters  NAA, NLK, NAU, NPM, NWC  NWC induces the strongest precipitation signature  Simulated several hypothetical transmitters distributed broadly in geomagnetic latitude and operating at a wide range of frequencies.  Investigated the relationship between transmitter location, operating frequency and radiated power   H (source location) directly proportional to resonant energy   inversely proportional to resonant energy  Location, location, location!  Future work: compare predictions with data