Science Goal and Approach Sessions

1
H1Local Helioseismology I Current Issues

• Science Goal and Approach Sessions
• Chair(s) Kosovichev/Toomre
• Status draft

2
S-2 Science questions and tasks

• Local helioseismology already provides
  unprecedented views of the Sun's interior 3D
  structures and flows, sunspots, active regions,
  and even the far-side activity. These all remain
  critical areas for achieving the HMI science
  objectives.

3
S-2 Science questions and tasks

• What are the primary targets and most critical
  issues of these investigations?
• How can we extend the local helioseismology
  measurements through the convection zone?
• What is needed to understand small-scale magnetic
  fields, sunspots, and active region?
• How best can we image the tachocline and 3D
  structures?

4
S-2 Science questions and tasks

• What is needed to adequately measure the
  meridional and other 3D flows?
• How do we link the helioseismic measurements on
  different scales to the SDO photospheric, coronal
  and irradiance data?
• How can we develop the predictive capabilities of
  local helioseismology?

5
S-3 Science context

• What progress has already been made?
• Where do we expect answers before launch?
• Where do we plan to concentrate our efforts?

6
S-3 Science context - Agenda

• 315-330 Turbulent magnetohydrodynamics of the
  Sun big questions and key targets for HMI -
  J.Toomre
• 330-340 Time-distance helioseismology of the
  deep interior - T.L.Duvall, Jr
• 340-350 Local helioseismology at small scales -
  T.Sekii
• 350-400 Ring-diagram flow maps from large to
  small tiles - D.Haber
• 400-410 Far-side holography imaging for HMI -
  P.H.Scherrer
• 410-420 European Local Helioseismology and
  HELAS - L.Gizon
• 420-435 General discussion
• 435-445 Summary, Organization of the Local
  Helioseismology Working Group - A.G.Kosovichev

7
S-4 Implementation

• What do we need to make progress on the science
  questions in general?
• Should a TRT focused topic be made?
• Discussion point
• Suggestion for Helioseismology Working groups
• Time-Distance Holography
• Global Helioseismology Rings
• Local Helioseismology Comparison (LoHCo)
• Observables, models, codes, resources,
  techniques, people
• Schedules, meetings, splinters, etc.

8
A Possible Schedule for discussion

• 17 November 2005 Announce the meeting, identify
  and advertise sessions and leaders. Request
  comments and suggestions on the Session Templates
  and the Session agenda from the session leaders
  and science team (respectively).
• 1 December 2005 Session leaders return comments
  and suggestions for the Session Template to the
  SOC (aia-hmi_soc_at_quake.stanford.edu)
• 15 December 2005 SOC circulates skeleton
  templates, agenda, and revised sessions
• 9 January 2006 SOC and the Session Leaders
  prepare the final session agenda and identify key
  session participants SOC organizes a telecon
  discussion of the final agenda
• 6 February 2006 Pre-meeting drafts of templates
  circulated to teams
• 13-17 February 2006 discussions during science
  team meeting
• implementation of the Science Plan, analysis
  techniques and computer codes
• additions and changes to the Science Plan
• implementation schedule, commitments and
  requirements
• suggestions for working groups
• request input for the Science Plan and HMI Data
  Analysis Pipeline from the participants.
• 24 February 2005 Session Leaders send the
  completed Session Report (following the Template)
  and first draft of the updated Science Plan
  sections (including suggestions for the HMI Data
  Analysis Pipeline) to the science team organize
  a discussion telecon
• 6 March 2006 Session Leaders submit the final
  Session Report and updated Science Plan to the
  SOC (aia-hmi_soc_at_quake.stanford.edu)
• 12 March 2006 a complete updated version of the
  HMI Science Plan is posted on meeting website
  comments from the entire HMI Science Team are
  requested
• 24 March 2006 the final updated HMI Science Plan
  is posted on the HMI web page