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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 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
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
CISM Advisory Council Meeting 4 March 2003
Magnetospheric Models
Lyon-Fedder-Mobarry Global Magnetospheric ModelJ. Lyon & M. Wiltberger Dartmouth & NCAR
Dartmouth Radiation Belt Model
M. K. Hudson, B. KressDartmouth, S. Elkington,LASP
Rice Convection Model
F. ToffolettoRice University
MI Coupling Model
W. LotkoDartmouth
Reconnection CodesJ. DrakeUniversity of MarylandB. 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 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
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 Couplingsubgrid 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
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