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Magnetospheric Modeling

Magnetospheric Modeling. Mary K. Hudson and the CISM Magnetospheric Modeling Team. Magnetospheric Modeling. Goal Take solar wind input and energetic particle flux and couple magnetospheric response with ionosphere. Magnetospheric Space Weather Impacts.

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Magnetospheric Modeling

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  1. Magnetospheric Modeling Mary K. Hudson and the CISM Magnetospheric Modeling Team

  2. Magnetospheric Modeling • Goal • Take solar wind input and energetic particle flux and couple magnetospheric response with ionosphere

  3. Magnetospheric Space Weather Impacts Space Weather Event Physical Consequence Technological Impact SSC Magnetosphere compressed Geosync S/C leaves msph Storms (CME-driven) Rapid inductive creation of S/C deep dielectric charging radiation belts SEUs, EVA hazard Ring current energization S/C charging, SP degradation SW Stream Interaction Relativistic electron S/C deep dielectric charging energization Substorms Ring current injection from S/C charging, SP degradation magnetotail Auroral currents intensify, GICs in transmission lines move to lower latitude Increased auroral precipitation, Thermospheric heating energization enhances S/C drag

  4. Magnetospheric Science Questions • Magnetosphere provides a shield to solar wind and energetic particles on the Earth; • Couples current flow at solar wind boundary to ionosphere • Macroscale • What is the flow of energy and momentum within the system • Radiation belt dynamics • Mesoscale • Structure of boundary layers, magnetopause • Auroral current systems, MI coupling • Microscale • Reconnection, particle acceleration • Modeling of entire system is required for predictive capability

  5. Reconnection Codes J. Drake University of Maryland B. Rogers, Dartmouth MI Coupling Model Lyon-Fedder-Mobarry Global Magnetospheric Model W. Lotko Dartmouth J. Lyon & M. Wiltberger Dartmouth & NCAR Rice Convection Model Dartmouth Radiation Belt Model F. Toffoletto Rice University M. K. Hudson, B. Kress Dartmouth, S. Elkington, LASP Magnetospheric Models

  6. Magnetospheric Products • Global MHD simulations driven by upstream solar wind input • Radiation belt fluxes (100 keV - 10's MeV electrons and protons) driven by MHD code input • Ring current ion and 1-100 keV electron fluxes specified by Rice Convection Model multifluid code coupled with MHD code • Subgrid model of auroral acceleration embedded in global MHD code • Synthetic aurora modelling, field line current coupling to the ionosphere from global MHD code

  7. Snapshot of density in noon-midnight meridian from MHD code simulation of Jan 15, 2000 CME-magnetic cloud interaction with Earth's magnetosphere. Simulation driven by upstream solar wind parameters measured by the ACE spacecraft at L1.

  8. The Rice Convection Model incorporates relative drift of species, hence ring current ions and electrons up to 0.5 MeV, given a magnetic field specification which can be provided by the LFM MHD code as well as a friction-MHD code. Coupling back to the MHD code will modify pressure evolution in the inner magnetosphere.

  9. Radiation belt electron flux vs. energy and L (geocentric radial distance in Earth radii) snapshots from initial (NASA AE8max model) to final state at 0440 UT on 15 Jul 2000, using MHD simulation fields to advance guiding center electron trajectories in the equatorial plane.

  10. EF in equatorial plane from MHD simulation of March 24, 1991 CME-interplanetary shock compression of magnetopause. Acceleration of ring of representative radiation belt electrons radially inward by inductive EF due to magnetopause compression is shown. No upstream solar wind parameters were available for this and similar events for the last solar maximum.

  11. Bastille Day storm Fe+11 trapping simulation

  12. MICoupling • subgrid physics • Heterogeneous coupling • - plasma • - neutral gas • - electrodynamics • Cross-scale coupling • - power deposition • depends on length scale • and activates other scales • Regional coupling • - active ionization and • depletion  feedback • - ion upwelling, outflow

  13. SAIC coupled to Odstrcil solar wind model for magnetic cloud

  14. Results from a LFM simulation based upon sythetic magnetic cloud parameters propogated from the solar surface to L1 by the coupled Linker and Odrisicil codes. The simulation was used to drive TING simulation so the inset is sythetic UV aurora from the LFM simulation.

  15. GIC Study – LFM currents mapped to geographic grid (March 19-20, 1999)

  16. Two way coupled Hall Conductivity

  17. Magnetospheric Team • Dartmouth College/ BU/ NCAR/ LASP • Mary Hudson - Co-director for magnetosphere • John Lyon - Global Magnetospheric MHD • Michael Wiltberger – Global Magnetospheric MHD • Brian Kress, Scot Elkington – MHD/Radiation Belt Dynamics • William Lotko – MI Coupling • Barrett Rogers – Magnetic Reconnection • Simon Shepherd – Ground-Induced Currents • Rice University • Frank Toffoletto - Rice Convection Model • Anthony Chan - Rice Convection Model • University of Maryland • James Drake - Magnetic Reconnection • Michael Shay – Magnetic Reconnection

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