CISM Advisory Council Meeting 4 March 2003 Magnetospheric Modeling Mary K. Hudson and the CISM Magnetospheric Modeling Team

CISM Advisory Council Meeting 4 March 2003 Magnetospheric Modeling Goal –Take solar wind input and energetic particle flux and couple magnetospheric response with ionosphere

CISM Advisory Council Meeting 4 March 2003 Magnetospheric Space Weather Impacts Space Weather Event Physical ConsequenceTechnological Impact SSC Magnetosphere compressed Geosync S/C leaves msph Storms (CME-driven) Rapid inductive creation of S/C deep dielectric charging radiation beltsSEUs, 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

CISM Advisory Council Meeting 4 March 2003 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

CISM Advisory Council Meeting 4 March 2003

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

CISM Advisory Council Meeting 4 March 2003 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 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

CISM Advisory Council Meeting 4 March 2003 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.

CISM Advisory Council Meeting 4 March 2003 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.

CISM Advisory Council Meeting 4 March 2003 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.

CISM Advisory Council Meeting 4 March 2003 E  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 E  due to magnetopause compression is shown. No upstream solar wind parameters were available for this and similar events for the last solar maximum.

CISM Advisory Council Meeting 4 March 2003 Bastille Day storm Fe+11 trapping simulation

CISM Advisory Council Meeting 4 March 2003 MI Coupling 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

CISM Advisory Council Meeting 4 March 2003 Magnetic field amplitude measured by GOES 9 geosynchronous spacecraft is compared with MHD code output at same location in the simulation domain. Excellent agreement with large solar wind pressure pulse compression of magnetopause inside geosynchronous orbit ~ 0200 UT on 11 Jan is evident. Discrepancy at earlier time reflects need to incorporate improved ring current (RCM) model.

CISM Advisory Council Meeting 4 March 2003 SAIC coupled to Odstrcil solar wind model for magnetic cloud

CISM Advisory Council Meeting 4 March 2003 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.

CISM Advisory Council Meeting 4 March 2003 GIC Study – LFM currents mapped to geographic grid (March 19-20, 1999)

CISM Advisory Council Meeting 4 March 2003 Two way coupled Hall Conductivity

CISM Advisory Council Meeting 4 March 2003 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

CISM Advisory Council Meeting 4 March 2003