Solar Physics With The Virtual Solar Observatory

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Solar Physics With The Virtual Solar Observatory

• Frank Hill The VSO Team

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The VSO Team

• Rick Bogart
• Alisdair Davey
• George Dimitoglou
• Joe Gurman
• Frank Hill
• Joe Hourclé

• Piet Martens
• Kevin Reardon
• Igor Suárez-Solá
• Karen Tian
• Steve Wampler
• Keiji Yoshimura

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Outline

• Solar physics data practices
• Introduction to the VSO
• Design
• Data sets
• Interface
• Shopping Cart
• API
• Community usage

• Science with the VSO
• Farside imaging and frontside activity
• Farside CMEs
• Subsurface flows solar wind speed
• Statistical study of active region life cycle
• Sunspot energetics

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Solar Physics Data Practices

• Average observational paper uses 4 to 6 data sets
  (sometimes 30)
• Multi-wavelength
• Multi-observable
• Time domain dominates
• Only one object
• Catalogs of features and events

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The Original Small Box
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(No Transcript)
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Data Sets
MLSO
RHESSI
Yohkoh
Digitized plates since 1915
GOES-12
SOLIS, FTS, O-SPAN
Nancay, Pic Du Midi
SOHO, TRACE, STEREO
MDI, GONG, Mt. Wilson, TON
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Interface
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Shopping Cart
Carts are permanently stored, retrievable, and
citable searches can be replicated.
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API
Provides link between VSO and other systems
IDL/SolarSoft, COSEC, EGSO, HelioScope,
AstroGrid, Aladin, VO.
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Community Usage
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Farside imaging and frontside activity
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Farside Coronal Mass Ejections
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Subsurface flows and solar wind speed
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Statistical study of active region life cycle
2. Surface evolution (magnetograms intensity
images)
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Sunspot energetics
4. Bright faculae near limb increase with spot
number.
5. Need multi-? observations for data to compute
sunspot energy budget.
1. Solar irradiance varies in antiphase with
sunspot number.
2. But spots are dark cool in the visible.
3. Ca K shows emission near spots.
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Space weather predictions
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1. Farside imaging 2. active region evolution
3. filament dynamics 4. flare observations 5.
CME observations 6. heliospheric magnetic field
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