HMI Data Products Plan and Status LWS Teams

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

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. LWS Teams Day JSOC Overview Page 2

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) LWS Teams Day JSOC Overview Page 3

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

Primary Science Objectives 1. 2. 3. 4. 5. 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. 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. 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. 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 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. LWS Teams Day JSOC Overview Page 5

HMI Science Analysis Plan HMI Data Processing Data Product Science Objective Tachocline Global Helioseismology Processing Internal rotation Ω(r, Θ) (0<r<R) Internal sound speed, cs(r, Θ) (0<r<R) Differential Rotation Local Helioseismology Processing Full-disk velocity, v(r, Θ, Φ), And sound speed, cs(r, Θ, Φ), Maps (0 -30 Mm) Activity Complexes Filtergrams Carrington synoptic v and cs maps (0 -30 Mm) Observables Doppler Velocity High-resolution v and cs maps (0 -30 Mm) Deep-focus v and cs maps (0 -200 Mm) Far-side activity index Line-of-sight Magnetograms Vector Magnetograms Continuum Brightness Line-of-Sight Magnetic Field Maps Near-Surface Shear Layer Active Regions Sunspots Irradiance Variations Magnetic Shear Flare Magnetic Configuration Flux Emergence Magnetic Carpet Coronal energetics Vector Magnetic Field Maps Large-scale Coronal Fields Coronal magnetic Field Extrapolations Far-side Activity Evolution Coronal and Solar wind models Brightness Images LWS Teams Day JSOC Overview Meridional Circulation Solar Wind Predicting A-R Emergence IMF Bs Events Version 1. 0 w Page 6

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

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

Helioseismology Heliographic Doppler velocity maps Filtergrams Doppler Velocity Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Ring diagrams Local wave frequency shifts Time-distance Tracked Tiles Cross-covariance Of Dopplergrams function Egression and Ingression maps Code: Doppler velocity, Lev 1 J. Schou S. Tomczyk Code: artificial data N. Mansour A. Wray R. Stein Status: needs improvements Status: in development LWS Teams Day JSOC Overview Internal rotation Ω(r, Θ) (0<r<R) Wave travel times Wave phase shift maps Internal sound speed, cs(r, Θ) (0<r<R) Full-disk velocity, v(r, Θ, Φ), And sound speed, cs(r, Θ, Φ), Maps (0 -30 Mm) Carrington synoptic v and cs maps (0 -30 Mm) High-resolution v and cs maps (0 -30 Mm) Deep-focus v and cs maps (0 -200 Mm) Far-side activity index Page 9

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

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

Time-Distance Helioseismology Full-disk velocity, v(r, Θ, Φ), And sound speed, cs(r, Θ, Φ), Maps (0 -30 Mm) Filtergrams Doppler Velocity Time-distance Tracked Tiles Cross-covariance Of Dopplergrams function Wave travel times Carrington synoptic v and cs maps (0 -30 Mm) High-resolution v and cs maps (0 -30 Mm) Deep-focus v and cs maps (0 -200 Mm) Code: fastrack R. Bogart, T. Duvall J. Zhao Status: needs improvements (remapping issues) LWS Teams Day JSOC Overview Code: crosscovariance 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: deepfocus maps T. Duvall A. Kosovichev J. Zhao Status: needs substantial development Page 12

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

Magnetic Fields Filtergrams Stokes I, V Line-of-sight Magnetograms Stokes I, Q, U, V Full-disk 10 -min Averaged maps Vector Magnetograms Fast algorithm Tracked Tiles Vector Magnetograms Inversion algorithm Line-of-Sight Magnetic Field Maps Vector Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Code: Stokes I, V, Lev 0. 5 V & LOS field J. Schou S. Tomzcyk Code: Stokes I, Q, U, V J. Schou S. Tomzcyk Status: in development LWS Teams Day JSOC Overview Page 14

Line-of Sight Magnetic Field Filtergrams Stokes I, V 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 LWS Teams Day JSOC Overview 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 15

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

Intensity Brightness Images Filtergrams Tracked full-disk 1 -hour averaged Continuum maps Continuum Brightness Synoptic Maps Solar limb parameters per image for Lev 0. 5 Code: Continuum Maps Schou Code: Averaged Continuum Maps Bush Code: Solar Limb Parameters, Lev 0. 5 used to make other Lev 1 products, Lev 2 for science goals Brightness feature maps Code: Brightness Feature Maps (European contribution) Code: Brightness Synoptic Maps Scherrer Status: in development R. Bush J. Kuhn Status: in development LWS Teams Day JSOC Overview Status: in development Page 17

Detail Example: Time-Distance Helioseismology Products • – – – – – – • – Full-disk synoptic flow maps: Area: from -60 to +60 deg in longitude and latitude (30 x 30 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: 30 x 30 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: 30 x 30 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. LWS Teams Day JSOC Overview Page 18

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) LWS Teams Day JSOC Overview Page 19

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). LWS Teams Day JSOC Overview Page 20