Page 1LWS Teams Day JSOC Overview HMI Data Products: Plan and Status

Page 2LWS Teams Day JSOC Overview Primary goal: origin of solar variability The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study the origin of solar variability and to characterize and understand the Sun’s interior and the various components of magnetic activity. HMI produces data to determine the interior sources and mechanisms of solar variability and how the physical processes inside the Sun are related to surface and coronal magnetic fields and activity.

Page 3LWS Teams Day JSOC Overview Key Features of HMI Science Plan Data analysis pipeline: standard helioseismology and magnetic field analyses Development of new approaches to data analysis Targeted theoretical and numerical modeling Focused data analysis and science working groups Joint investigations with AIA and EVE Cooperation with other space- and ground-based projects (SOHO, Hinode, PICARD, STEREO, RHESSI, GONG+, SOLIS, HELAS)

Page 4LWS Teams Day JSOC Overview HMI Major Science Objectives 1.B – Solar Dynamo 1.C – Global Circulation 1.D – Irradiance Sources 1.H – Far-side Imaging 1.F – Solar Subsurface Weather 1.E – Coronal Magnetic Field 1.I – Magnetic Connectivity 1.J – Sunspot Dynamics 1.G – Magnetic Stresses 1.A – Interior Structure NOAA 9393 Far- side

Page 5LWS Teams Day JSOC Overview 1.Convection-zone dynamics and solar dynamo –Structure and dynamics of the tachocline –Variations in differential rotation. –Evolution of meridional circulation. –Dynamics in the near-surface shear layer. 2.Origin and evolution of sunspots, active regions and complexes of activity –Formation and deep structure of magnetic complexes. – Active region source and evolution. –Magnetic flux concentration in sunspots. –Sources and mechanisms of solar irradiance variations. 3.Sources and drivers of solar activity and disturbances –Origin and dynamics of magnetic sheared structures and delta-type sunspots. –Magnetic configuration and mechanisms of solar flares and CME. –Emergence of magnetic flux and solar transient events. –Evolution of small-scale structures and magnetic carpet. 4. Links between the internal processes and dynamics of the corona and heliosphere –Complexity and energetics of solar corona. –Large-scale coronal field estimates. –Coronal magnetic structure and solar wind 5.Precursors of solar disturbances for space-weather forecasts –Far-side imaging and activity index. –Predicting emergence of active regions by helioseismic imaging. –Determination of magnetic cloud Bs events. Primary Science Objectives

Page 6LWS Teams Day JSOC Overview HMI Science Analysis Plan Magnetic Shear

Page 7LWS Teams Day JSOC Overview HMI module status and MDI heritage Doppler Velocity Heliographic Doppler velocity maps Tracked Tiles Of Dopplergrams Stokes I,V Continuum Brightness Tracked full-disk 1-hour averaged Continuum maps Brightness feature maps Solar limb parameters Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Line-of-sight Magnetograms Vector Magnetograms Fast algorithm Vector Magnetograms Inversion algorithm Egression and Ingression maps Time-distance Cross-covariance function Ring diagrams Wave phase shift maps Wave travel times Local wave frequency shifts Spherical Harmonic Time series Mode frequencies And splitting Brightness Images Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, sound speed, Maps (0-30Mm) Internal sound speed Internal rotation Vector Magnetic Field Maps MDI pipeline modules exist Standalone production codes in use at Stanford Research codes in use by team Codes to be developed at HAO Codes being developed in the community Codes to be developed at Stanford Primary observables Intermediate and high level data products

Page 8LWS Teams Day JSOC Overview JSOC - HMI Pipeline HMI Data Analysis Pipeline Doppler Velocity Heliographic Doppler velocity maps Tracked Tiles Of Dopplergrams Stokes I,V Filtergrams Continuum Brightness Tracked full-disk 1-hour averaged Continuum maps Brightness feature maps Solar limb parameters Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Line-of-sight Magnetograms Vector Magnetograms Fast algorithm Vector Magnetograms Inversion algorithm Egression and Ingression maps Time-distance Cross-covariance function Ring diagrams Wave phase shift maps Wave travel times Local wave frequency shifts Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Brightness Images Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Internal sound speed, c s (r,Θ) (0<r<R) Internal rotation Ω(r,Θ) (0<r<R) Vector Magnetic Field Maps HMI Data Data ProductProcessing Level-0 Level-1

Page 9LWS Teams Day JSOC Overview Helioseismology Code: Doppler velocity, Lev1 J.Schou S.Tomczyk Status: needs improvements Code: artificial data N. Mansour A. Wray R. Stein Status: in development Doppler Velocity Tracked Tiles Of Dopplergrams Filtergrams Egression and Ingression maps Time-distance Cross-covariance function Ring diagrams Wave phase shift maps Wave travel times Local wave frequency shifts Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Internal rotation Ω(r,Θ) (0<r<R) Heliographic Doppler velocity maps Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Internal sound speed, c s (r,Θ) (0<r<R)

Page 10LWS Teams Day JSOC Overview Global helioseismology Code: project J. Schou Status: ready to port Code: qdotprod J.Schou Status: ready to port Code: med-l peak bagging J.Schou High-l ridge fitting, E. Rhodes Status: needs improvements Code: sound- speed inversions A.Kosovichev Status: ready to port Code: rotation inversion J.Schou R. Howe Status: ready to port Doppler Velocity Filtergrams Internal rotation Ω(r,Θ) (0<r<R) Heliographic Doppler velocity maps Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Internal sound speed, c s (r,Θ) (0<r<R)

Page 11LWS Teams Day JSOC Overview Ring Diagrams Doppler Velocity Tracked Tiles Of Dopplergrams Filtergrams Ring diagrams Local wave frequency shifts Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Code: fastrack R.Bogart, J.Toomre D. Haber B. Hindman Status: needs improvements Code: power spectrum R.Bogart Status: ready to port Code: sensitivity kernels A.Birch Status: in development Code: inversions J.Toomre, D.Haber, B.Hindman Status: needs improvements Code: ring fitting S.Basu, F.Hill, J.Toomre, D.Haber, B.Hindman Status: needs improvements Need $$

Page 12LWS Teams Day JSOC Overview Time-Distance Helioseismology Doppler Velocity Tracked Tiles Of Dopplergrams Filtergrams Time-distance Cross-covariance function Wave travel times Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Code: fastrack R.Bogart, T.Duvall J.Zhao Status: needs improvements (remapping issues) Code: cross- covariance T.Duvall J.Zhao Status: needs improvements Code: travel time fitting T.Duvall J.Zhao S.Couvidat Status: needs improvements Code: sensitivity kernels A.Kosovichev J.Zhao A.Birch Status: needs improvements Code: inversions A.Kosovichev J.Zhao, A.Birch S.Couvidat J.Toomre B.Hindman Status: needs improvements Code: deep- focus maps T.Duvall A.Kosovichev J.Zhao Status: needs substantial development

Page 13LWS Teams Day JSOC Overview Acoustic Holography Doppler Velocity Tracked Tiles Of Dopplergrams Filtergrams Egression and Ingression maps Wave phase shift maps Far-side activity index High-resolution v and c s maps (0-30Mm) Code: fastrack R.Bogart D.Braun C.Lindsay Status: needs improvements (field-effect corrections) Code: egression- ingression D.Braun C.Lindsay Status: needs improvements Code: phase shifts D.Braun C.Lindsay Status: needs improvements (showglass corrections) Code: sensitivity kernels A. Birch Status: in development Code: holographic inversions A.Birch Status: in development Code: Far-side imaging P.Scherrer C.Lindsay D.Braun Status: needs improvements Inversions

Page 14LWS Teams Day JSOC Overview Magnetic Fields Stokes I,V Filtergrams Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Line-of-sight Magnetograms Vector Magnetograms Fast algorithm Vector Magnetograms Inversion algorithm Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Vector Magnetic Field Maps Code: Stokes I,V, Lev0.5 V & LOS field J. Schou S. Tomzcyk Status: in development Code: Stokes I,Q,U,V J. Schou S. Tomzcyk Status: in development

Page 15LWS Teams Day JSOC Overview Line-of Sight Magnetic Field Stokes I,V Filtergrams Line-of-sight Magnetograms Line-of-Sight Magnetic Field Maps Synoptic Magnetic Field Maps Magnetic Footpoint Velocity Maps Code: LOS magnetograms J. Schou S. Tomzcyk R. Ulrich (cross calib) Status: in development Code: LOS magnetic maps (project?) T. Hoeksema R. Bogart Status: in development Code: Synoptic Magnetic Field Maps T. Hoeksema X. Zhao R. Ulrich Status: in development Code: Velocity Maps of Magnetic Footpoints Y. Liu G. Fisher Status: in development

Page 16LWS Teams Day JSOC Overview Vector Magnetic Field Filtergrams Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Vector Magnetograms Fast algorithm Coronal magnetic Field Extrapolations Vector Magnetic Field Maps Code: fastrack R. Bogart Status: needs modifications for fields Code: Vector Field Fast and Inversion Algorithms J. Schou S. Tomzcyk Status: in development Code: Vector Field Maps T. Hoeksema Y.Liu Status: in development Code: Coronal Field Extrapolations & Ambiguity issue T.Hoeksema Y.Liu, X.Zhao C. Schrijver P.Goode T.Metcalf K.D.Leka Status: in development Code: Coronal Magnetic Field Topological Properties J.Linker V. Titov Status: needs implementation Code: Solar Wind Models X.Zhao K.Hayshi J.Linker P.Goode V.Yurchishin Status: in development Coronal and Solar wind models Vector Magnetograms Inversion algorithm Need $$

Page 17LWS Teams Day JSOC Overview Intensity Filtergrams Continuum Brightness Brightness Images Code: Continuum Maps Schou Status: in development Code: Solar Limb Parameters, Lev0.5 used to make other Lev1 products, Lev2 for science goals R. Bush J. Kuhn Status: in development Code: Brightness Feature Maps (European contribution) Status: in development Code: Averaged Continuum Maps Bush Status: in development Solar limb parameters per image for Lev0.5 Brightness Synoptic Maps Tracked full-disk 1-hour averaged Continuum maps Code: Brightness Synoptic Maps Scherrer Status: in development Solar limb parameters Brightness feature maps

Page 18LWS Teams Day JSOC Overview Detail Example: Time-Distance Helioseismology Products Full-disk synoptic flow maps: –Area: from -60 to +60 deg in longitude and latitude (30x30 deg tracked regions, sampling TBD) –Depth: 0-30 Mm (~ 20 distances) –Cadence: 3 per day –Resolution: 0.2 deg per pixel –Comment: systematic errors for sound-speed maps may be too large; usefulness is unclear – suggestion: descope Carrington synoptic maps: –Central meridian flow maps made from the full-disk maps High-resolution flow and sound-speed maps of tracked AR –Area: 30x30 deg –Depth: 0-30 Mm –Cadence: 8 hours (with a 2-hour shift? Need to study this option) –Resolution: 0.06 deg/pixel –Track areas of all AR in NOAA from -60 to +60 longitude (including periods prior flux emergence and after disappearance) –Need matching vector magnetograms High-resolution flow and sound-speed maps of flaring AR –Area: 30x30 deg –Depth: 0-30 Mm –Cadence: 4 hours (with a 1-hour shift) –Resolution: 0.06 deg/pixel –Track AR with NOAA probability of X-class flare > 30% ? (need selection criteria) –Need corresponding high-cadence vector magnetograms Deep-focus flow maps –Keep as research topic, include in pipeline when ready. Additional funding/FTE required.

Page 19LWS Teams Day JSOC Overview Organization of TD data analysis Two parallel techniques: 1.Gabor wavelet fitting for phase and group travel times + ray-path inversions 2.Cross-correlation measurement of reference travel times + Born inversions –Two data analysis options: 1.Standard pipeline processing with standard fitting and inversion parameters 2.Interactive processing (Junwei’s IDL widgets) – should be able to import intermediate data from pipeline processing (e.g. travel times for experimental inversions)

Page 20LWS Teams Day JSOC Overview Summary HMI will provide key data to study the Sun’s dynamics and magnetism: subsurface flow maps and photospheric vector magnetic fields. The HMI data analysis plan includes a standard pipeline processing and interactive data analysis tools. The analysis pipeline is being developed by the Co-I team, using existing techniques and software. However, to fully utilize the science potential of HMI additional funding is necessary for Co-I’s teams (in particular, for helioseismic imaging of the deep interior/tachocline, and coronal/heliospheric magnetic field analysis and models).