Goals for local helioseismology

1. Goals for local helioseismology A. Kosovichev HMI Team Meeting

2. HMI Major Science Objectives 1.B – Solar Dynamo 1.J – Sunspot Dynamics 1.C – Global Circulation 1.I – Magnetic Connectivity 1.A – Interior Structure 1.D – Irradiance Sources 1.E – Coronal Magnetic Field 1.H – Far-side Imaging NOAA 9393 Far-side 1.F – Solar Subsurface Weather 1.G – Magnetic Stresses HMI Team Meeting

3. Doppler Velocity Line-of-sight Magnetograms Vector Magnetograms Continuum Brightness HMI Science Analysis Plan HMI Data Processing Data Product Science Objective Tachocline Global Helioseismology Processing Internal rotation Ω(r,Θ) (0<r<R) Meridional Circulation Filtergrams Internal sound speed, cs(r,Θ) (0<r<R) Differential Rotation Near-Surface Shear Layer Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Local Helioseismology Processing Activity Complexes Active Regions Carrington synoptic v and cs maps (0-30Mm) Sunspots Irradiance Variations High-resolution v and cs maps (0-30Mm) Observables Magnetic Shear Deep-focus v and cs maps (0-200Mm) Flare Magnetic Configuration Flux Emergence Far-side activity index Magnetic Carpet Line-of-Sight Magnetic Field Maps Coronal energetics Large-scale Coronal Fields Vector Magnetic Field Maps Solar Wind Coronal magnetic Field Extrapolations Far-side Activity Evolution Predicting A-R Emergence Coronal and Solar wind models IMF Bs Events Version 1.0w Brightness Images HMI Team Meeting

4. SDO Local helioseismology methods Time-distance helioseismology Ring-diagram analysis Acoustic holography HMI Team Meeting

5. Local helioseismology investigation cycle Tasks Data Interpretation Models Results Data analyses Tests Data Inversions HMI Team Meeting

6. Local helioseismology tasks • Large-scale synoptic mapping of the solar interior: solar-cycle evolution and global circulation • Multi-scale convection • Magnetic flux emergence • Lifecycle of active regions • Structure and dynamics of sunspot • Shear flows and conditions for flares and CME HMI Team Meeting

7. Data requirements • Uninterrupted series of Dopplergrams • Good oscillation signal in regions of strong magnetic field • Secondary data • Magnetograms • Oscillation data in other spectral lines for understanding wave excitation and interaction with magnetic fields (e.g.“showerglass” effect, Charles Lindsey) HMI Team Meeting

8. Models for data analysis • Acoustic ray theory (time-distance, holography) • Born approximation (time-distance, Aaron Birch will talk about recent progress) • Uncoupled plane waves (ring diagrams) HMI Team Meeting

9. Data analyses A standard procedure for measuring travel-time perturbations has been developed (Tom Duvall). Two observing schemes: HMI Team Meeting

10. Data inversion • Solving very large ill-conditioned linear systems • Methods • LSQR (Michael Saunders, SCCM) • Multi-channel deconvolution (B. Jacobsen et al, Sebastien Couvidat will give examples) Need to develop: • Method for estimating the null space (what we do not see) to develop optimal observing schemes • Cross-validation methods HMI Team Meeting

11. Tests • Intercomparison (LoHCo) • Hare-and-Hounds inversion exercise (initial results - Sebastien Couvidat) • Numerical modeling of wave propagation – currently, this is the most important problem for validating results of local helioseismology and developing robust analysis methods; first steps are being made. HMI Team Meeting

12. Results Synoptic flow map from ring diagrams and time distance Carrington rotation 1948, depth 1.5 Mm HMI Team Meeting

13. HMI Team Meeting

14. A search for the relationship between flaring activity and subphotospheric flows: M4.3 flare, March 28, 2001, 11:20-12:40 UT HMI Team Meeting

15. Interpretation • Derive various properties (meridional circulation, vorticity, kinetic helicity etc) • Statistical analysis • Compare with theoretical models and numerical simulations • Data assimilation, inverse modeling, forecast HMI Team Meeting