11/10/05 H1:Local Helioseismology I: Current Issues Science Goal and Approach Sessions Chair(s): Kosovichev/Toomre Status: [draft]

11/10/05 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.

11/10/05 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?

11/10/05 S-3: Science context - Agenda 3:15-3:30 Turbulent magnetohydrodynamics of the Sun: big questions and key targets for HMI - J.Toomre 3:30-3:40 Time-distance helioseismology of the deep interior - T.L.Duvall, Jr 3:40-3:50 Local helioseismology at small scales - T.Sekii 3:50-4:00 Ring-diagram flow maps: from large to small tiles - D.Haber 4:00-4:10 Far-side holography imaging for HMI - P.H.Scherrer 4:10-4:20 European Local Helioseismology and HELAS - L.Gizon 4:20-4:35 General discussion 4:35-4:45 Summary, Organization of the Local Helioseismology Working Group - A.G.Kosovichev

11/10/05 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?

11/10/05 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?

11/10/05 S-4: Implementation What do we need to make progress on the science questions in general? –Should a TR&T 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.

11/10/05 S-4: Implementation –Schedules, meetings, splinters, etc. Global Helioseismology & Rings (Stanford, April 10-14, 2006 ?) Time-Distance & Holography (Stanford, July 10-14, 2006 ?) Local Helioseismology Comparison (LoHCo) (Tucson, December 2006 ?) –Observables, models, codes, resources, techniques, people …

11/10/05 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- 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 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- 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

11/10/05 Juri: –Why no clear detection of the giant cells? Need 3-components of flow fields, supergranulation may hide GC flows of 50 m/s. –Meridional circulation – multi-celled structure? Crucial for dynamo flux transport. Need to probe deeper. –Flows near Magnetism. Who pushes them around? Complex mode conversion. Continuous subsurface mapping – fast analysis pipeline. Flow near filaments. –Theory and simulation of large-scale flows

11/10/05 Tom: –Chou-Serebryanky; Magnetic field at the base of the convection zone –Deep flow measurements –Measuring convective times from simulations. RMD =100 m/a

11/10/05 Takashi –Solar-B SOT – SDO high-resolution + broader coverage, simultaneous observations in magnetic and non-magnetic lines –Propagation of waves in magnetized fluid: wavelength is comparable to the fluxtube size –Can we observe kernels? (Duvall et al) – How to merge f- and p-mode data?

11/10/05 Deborah –Take into account the spherical nature of the Sun –Small tiles 30 deg –Small tiles science Flows around eruptive filaments Flows beneath active regions Flows associated with supergranulations and giant cells –Large tiles Meridional flows and zonal flows lon. Structure –High-resolution f- and p1 rings –Compare with global analysis (zonal flows) –Tasks: multiple ridge fits, tracking, 3D inv, spher.corr., magnetic field, non-Lorentzian

11/10/05 Laurent –Coordinate and consolidate European research –Facilitate preparation for SDO and Solar Orbiter –Distribute data analysis tools –Meetings:SOHO-17, 2007, Gottingen, August 20-24, –September 25-27, 2006 Nice –Local helioseismology roadmap

11/10/05 Phil –Farside Graphic Viewer –Center-to-Limb Variations is a challenge