Upload
roger-malone
View
222
Download
2
Tags:
Embed Size (px)
Citation preview
Klimchuk Matrix (2000)
Model Multi-polar
Flux Rope
Sheared NL
Converg. Flow
Recon. Timing
Recon. Location
Mass Distrib.
Breakout Y NR Y NR at/before above NR
Flux Rope NR Y Y Y1 after1 below NR
NR2 at/after2
Tether Cutting
NR NR Y NR at/before below NR
Flux Injection
NR Y NR NR NR NR NR
Mass Loading
NR NR NR NR NR NR cavityand/or
prominence
What are the key observations that can discriminate among the models?
Pre-event solar atmospherePre-event solar atmosphere CME AccelerationCME Acceleration
Vector BChromospheric fieldPhotospheric flowsMagnetic morphologyEmerging/canceling fluxRole of reconnectionRole of flares Role of filamentsMagnetic complexityHelicity evolutionFluxrope formationTriggering phenomena …
Accurate H-T and V-T profilesLocation of peak accelerationRole of solar windRelationship to magnetic cloudsInteraction with IP medium Flare vs. prominence divideRole of helicity (expulsion?)Changes in magnetic topologyEruption of sheared core fieldTiming/location of reconnectionProduction of shocksWave activity …
Modeling
Initial + boundary conditionsPhysical assumptionsDriving mechanismambient conditions
ReconnectionHeating, Cooling
Particle accelerationShock formation
…
Ultimate challenge: determine key observational/modeling overlaps and utilize these to provide most appropriate I.C.s and most useful comparisons of model outputs
Understanding the CME process observationallyUnderstanding the CME process observationally
Pre-event solar atmospherePre-event solar atmosphere CME AccelerationCME Acceleration
Observational needs: high cadence vector B high cadence continuum H filament obs. (inc. Doppler)
Modeling needs: include reconnection physics (particles?) inc. observed field configurations and evolution investigate role of emerging/canceling flux incorporate flow fields track helicity ….
Observational needs: high cadence low-to-high coronal multi-
wavelength observations stereoscopically derived morphology and
velocity evolution
Modeling needs: specify factors which determine acceleration identify correct boundary conditions how do models distinguish between fast and slow events identify model discriminators in the data
How do we define a realistic challenge and how do we meet it?How do we define a realistic challenge and how do we meet it?3 approaches:
- wait until spatial, temporal resolution and source region complexity can be incorporated
- Tackle in detail an individual event (e.g. 1997 May 12)
- select 2-3 common phenomena which can be realistically incorporated into the ‘generic’ models
e.g. kinking,
failed-partial-full eruption, reformation of pre-eruption configuration
Non-starter
Providing great insight and driving model development
Broader application to common processes describing events
Example template of dialog matrix: models
The Matrix ReloadedModel M1 (2.5D) M2 (3D) … …
Basic BC
Basic Geom. Arcade Fluxrope multipolarBasic concept
Driving force shear Loss of
equilibrium Reconnection
above
B field Y (vector) YH / He 1083 dynamics
EUV/X-ray Y (morphology)
M
Coronagraph Y YSolar Wind ?
Particles NR
Assumptions/challenges
Sensitivity tests
Observational needs
Shear profile
Definition
of Model
Observational
input/comparison
Improving
models
Example template of dialog matrix: observations
The Matrix ReloadedObservation Magnetic Field Coronal
(EUV/X-ray)Coronagraph Solar Wind …
f-o-v/resolution
cadence
morphology
dynamics
Energy release
…
Pre-eruption
Post-eruption
Flow maps
Topology
Assumptions/challenges
coalignment
Control groups
…
Observational
characteristics
Relationship
to model
parameters
Improving
observations
Dialog template would have additional fields for
• Definitions and nomenclature
• Brief discussions • Physical quantities: input data/ parameters, output observables, methods for direct comparisons• Specify the metric and basis for comparisons
• Key references
• Point-counterpoint• Emphasis on specific argument and evidence; new observations needed to resolve issues