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