Transcript P2_Kosovichev.HMIScience.ppt

HMI Science Goals
Alexander Kosovichev & HMI Team
HMI/AIA Science Team Meeting, 2006
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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.
HMI/AIA Science Team Meeting, 2006
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Illustration of solar dynamo
HMI/AIA Science Team Meeting, 2006
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Primary Science Objectives
1. Convection-zone dynamics and solar dynamo
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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
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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
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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
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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
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Far-side imaging and activity index.
Predicting emergence of active regions by helioseismic imaging.
Determination of magnetic cloud Bs events.
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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
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Farside
1.G – Magnetic Stresses
HMI/AIA Science Team Meeting, 2006
1.F – Solar Subsurface Weather
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HMI/AIA Science Team Meeting, 2006
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HMI Science Analysis Plan
HMI Data
Processing
Data Product
Science Objective
Global
Helioseismology
Processing
Internal rotation Ω(r,Θ)
(0<r<R)
Tachocline
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 (0-30Mm)
Activity Complexes
Filtergrams
Carrington synoptic v and cs
maps (0-30Mm)
Observables
Doppler
Velocity
High-resolution v and cs
maps (0-30Mm)
Deep-focus v and cs
maps (0-200Mm)
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
HMI/AIA Science Team Meeting, 2006
Meridional Circulation
Solar Wind
Predicting A-R Emergence
IMF Bs Events
Version 1.0w
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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 groundbased projects (SOHO, Solar-B, PICARD,
STEREO, RHESSI, GONG+, SOLIS, etc)
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