I: C1/M8/C10 Transients: Drivers

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I C1/M8/C10 Transients Drivers Destabilization

• Chair(s) Golub Nitta
• Status draft/review/final

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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.

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II Science questions and tasks (1)

• Primary scientific question
• How does the magnetic field change due to
  eruptions?
• What is the mapping of the low corona and the
  CME?
• What is the relation between large-scale and
  active region magnetic fields in CME initiation?
• How are particles accelerated in the corona?
• Are there multiple acceleration mechanisms?
• What is the relation between particles
  precipitating into the low atmosphere and those
  escaping from the Sun?

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II Science questions and tasks (2)

• SDO/AIA science tasks
• Task 2 Evolution of transients (Session C1/M8)
• Task 1 Unstable field configurations and
  initiation of transients (Session C1/M8)
• Task 3 Early evolution of CMEs
• Detect first brightenings and motions.
• Associate dimming regions with B and characterize
  CMEs.
• Task 4 Particle acceleration
• Find conjugate foot-points.
• Detect shocks.
• Study regions closer to the reconnection region.

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III Science context (1)

• STEREO will provide better understanding of the
  link between Earth-directed halo CMEs and 1-2 MK
  coronal structures.
• By the time of SDO launch, the two STEREO
  spacecraft will be separated by 90 degrees, and
  start to have good visibility of CMEs launched
  parallel to the Sun-Earth line.
• In combination with Solar-B/EIS and XRT, it will
  become possible to distinguish waves from
  ejections, and to understand the link between
  disturbances at 1-2 MK with those at high T.

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III Science context (2)

• More and more realistic simulations will make it
  possible to understand eruptions in terms of
  physics.
• Combination of simulations of magnetic
  reconnection and flux emergence and cancellation
  will pin-point CME initiation mechanisms at least
  on an event by event basis.
• Combination of MHD and particle code simulations
  will show us likely locations of particle
  acceleration.

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III Science context (3)

• Where do we expect/plan to make SDO contribute
  most efficiently and substantially, because of
  SDOs capabilities or timing?
• SDO will clarify how important magnetic
  reconnection is in initiation and early evolution
  of CMEs because of broad temperature coverage and
  simultaneous observations of bremsstrahlung and
  magnetic field.
• SDO will show us the origin of coronal waves and
  dimming because of the broad temperature
  coverage, high time resolution and full-disk
  coverage.

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IV Science investigation

• Identify hurdles, bottlenecks, uncertainties
• Locating and characterizing the reconnection
  region is difficult because of its predicted low
  emission.
• Observing pre-eruption flux ropes can be tricky
  because of their possible low twists combined
  with projection effects. STEREO carries no
  magnetographs.
• After SOHO, the lack of coronagraphs at fixed
  view points (which STEREO does not have) will
  make it hard to associate the low corona with
  CMEs.
• After RHESSI, no high-energy instruments are
  available. In particular, we will have no
  information on ion acceleration, which is
  essential for understanding of particle
  acceleration.