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HMI Science Goals

HMI Science Goals. Alexander Kosovichev & HMI Team. Primary goal: origin of solar variability.

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HMI Science Goals

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  1. HMI Science Goals Alexander Kosovichev & HMI Team

  2. 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.

  3. Illustration of solar dynamo

  4. Primary Science Objectives • 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-sideimaging and activity index. • Predicting emergence of active regions by helioseismic imaging. • Determination of magnetic cloud Bs events.

  5. 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

  6. 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

  7. 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, Solar-B, PICARD, STEREO, RHESSI, GONG+, SOLIS, etc)

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