Upload
lacey-kidd
View
25
Download
3
Embed Size (px)
DESCRIPTION
I: C1/M8 /C10 Transients: Drivers & Destabilization. Chair(s): Golub & Nitta Status: [draft/ review /final]. Schedule. 17 November 2005: draft sheets I, II to teams, requesting input for sheets III and IV - PowerPoint PPT Presentation
Citation preview
[C1] 1
SDO/AIA science plan: prioritization and implementation:
Five Objectives in 10 steps
I: C1/M8/C10 Transients: Drivers & Destabilization
Chair(s): Golub & Nitta
Status: [draft/review/final]
[C1] 2
Schedule
17 November 2005: draft sheets I, II to teams, requesting input for sheets III and IV
24 November 2005: completed sheets I-IV for review to teams, requesting input for sheets V-VI
8 December 2005: team input received for sheets V-VI 19 December 2005: draft of sheets VII-VIII to teams 9 January 2006: team comments received for sheets VII-
VIII 6 February 2006: draft ‘Science plans’ on meeting
website, with sheets IX-X filled out by team leads (or teams after telecons)
13-17 February 2006: discussions during science team meeting discuss and complete pages IX-X.
17 February: completed ‘Science plans’ on line.
[C1] 3
II: Science questions and tasks (1)
Primary scientific question: What types of magnetic field evolution lead
to instabilities and transients? What is the role of helicity injection and transfer? How does emerging flux interact with pre-existing
B? How is the stored magnetic released?
Is there a role for flux ropes? Where and how does reconnection occur?
[C1] 4
II: Science questions and tasks (2)
SDO/AIA science tasks: Task [1]: Unstable field configurations and
initiation of transients Find pre-eruption signatures of, e.g., tether-cutting or
breakout reconnection. Is braiding or sigmoid formation an eruption indicator? How do we best observe and use coronal dimming?
Task [2]: Evolution of transients Find signatures of inflow and outflow, cusps, patchiness
of reconnection. Determine how much flux participates in reconnection
episodes.D. McKenzie Overview Presentation
Task [3]: Early evolution of CMEs (Session C10) Task [4]: Particle acceleration (Session C10)
[C1] 5
III: Science context
Solar-B is likely to provide improved knowledge of locations of reconnection sites, inflows and outflows and local magnetic structure (modeled). Combination of XRT, EIS and B-extrapolations.
STEREO should provide improved knowledge of global configuration, in both plasma and field, and relation to properties of eruption. e.g., two magnetic configurations (normal and
inverse) vs. CME speed. Flux rope – ab initio vs. formed during event
[C1] 6
III: Science context (cont.)SDO will provide unique global coverage of: Pre-eruption coronal topology Magnetic field structure Event initiation and early evolution
Y. Su Presentation on shear change
How SDO data can be used: From B maps determine null points, separatrices or
QSLs. EUV channels provide imaging temperature (DEM) maps
of corona and its evolution. Locate and compare first brightenings and energy
release sites vs. global conditions (multi-polarity, helicity, etc,).
[C1] 7
III: Science context (cont.)
How to use SDO: Evolution of the full magnetic configuration. Determination of coronal B and comparison with EUV
observations. Observe T-slices of coronal structure, to follow all of
the plasmas as f(t). Need to know the large-scale field
Is “breakout” configuration a necessary condition? Systematic observations of pre-CME phase:
Flux tube present or not? Role of kink instability?Fludra/Harrison Presentation on CME Detection
[C1] 8
IV: Science investigation
Hurdles, bottlenecks, uncertainties: Parameters of flare trigger are unknown:
location, size, temperature, density. Consequences of energy release and particle
acceleration are visible (flare ribbons, chromospheric evaporation, heated plasma) but energy release site is not directly observed.
Large gap remains between B-extrapolations and observed coronal structure; not clear how to make progress.
[C1] 9
IV: Science investigation (cont.)
Hurdles, bottlenecks, uncertainties (cont.): What coronagraph observations will be
available? SOHO? STEREO? Other? Need to study tradeoffs for AIA: Number of
channels vs. image cadence vs. complexity of planning.