HMI – Synoptic Data Sets

HMI – Synoptic Data Sets HMI Team Meeting Jan. 26, 2005 Stanford, CA

Synoptic Data Sets - Helioseismology • Synoptic maps of mass flows and sound-speed perturbations in the upper convection zone for each Carrington rotation with a 2-degree resolution, from averages of full disk time-distance maps; • Synoptic maps of horizontal flows in the upper convection zone for each Carrington rotation with a 5-degree resolution from ring-diagram analyses; • Higher-resolution maps zoomed on particular active regions, sunspots and other targets, obtained with 4-8-hour resolution for up to 10-day transits; • Deep-focus maps covering the whole convection zone depth, 0-200 Mm, with 10-15 degree resolution; • Farside images of travel-time perturbations associated with large active regions every 12 hours.

Synoptic Data Sets • The traditional line-of-sight component of the magnetic flux is produced as a co-product with the Doppler velocity. Products include synoptic charts updated daily at low, medium, and high resolution. Charts will be constructed at 15 degree offsets from central meridian and adjusted for differential rotation. Synoptic frames available on demand. • Synoptic products computed for the coronal and heliospheric field will also be produced, archived, and distributed. • HMI will produce several standard data series of the vector magnetic field. A simple ‘magnetograph mode’ analysis will be computed continuously in real time for large scale coronal modeling and other space weather applications. HMI will provide tracked and full-disk vector magnetic field, filling factor, and thermodynamic parameters of photospheric plasma within reasonable errors. • Observations of the continuum intensity near the HMI spectral line will give a very useful measure of spot, faculae area and other sources of irradiance.

Global Helioseismology Processing HMI Data Processing Data Product Science Objective Tachocline Internal rotation Ω(r,Θ) (0<r<R) Meridional Circulation Local Helioseismology Processing 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) Activity Complexes Active Regions Carrington synoptic v and cs maps (0-30Mm) Sunspots Doppler Velocity Irradiance Variations High-resolution v and cs maps (0-30Mm) Observables Deep-focus v and cs maps (0-200Mm) Flare Magnetic Configuration Line-of-sight Magnetograms Flux Emergence Far-side activity index Magnetic Carpet Line-of-Sight Magnetic Field Maps Vector Magnetograms Coronal energetics Large-scale Coronal Fields Vector Magnetic Field Maps Solar Wind Continuum Brightness 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 Science Analysis Plan Magnetic Shear

HMI Data “Minimum” energy method (Metcalf, 1994) “Structure minimization” method (Georgoulis et al, 2004) 1. ILCT (Welsch et al, 2004) 2. “The minimum energy fit” (Longcope, 2004) 3. “Induction equation” (Kusano et al, 2002) 1. Optimization approach (Wheatland et al, 2000) Coronal magnetic fields. (NLFFF, MHD) Plasma flow. Synoptic maps PFSS & Hybrid models Heliospheric magnetic field Connectivity & separatrix Energy flux through the photosphere Helicity flux through the photosphere Topology structure Dynamical evolution MHD simulation Surface flow effect Solar transients Prediction of IMF & solar wind speed Empirical estimate; MHD simulation Emerging flux effect MHD simulation

HMI – Synoptic Data Sets