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Solar Image Processing: A Multiscale View
Solar Image Processing: A Multiscale View
C. Alex YoungNASA/GSFC
C. Alex YoungNASA/GSFC
UCLA - IPAM (January 28, 2004)
UCLA - IPAM (January 28, 2004)
OutlineOutline
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
OutlineOutline
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
The high energy sun.The high energy sun.
20 Jan 2000 Solar FlareBATSE and COMPTEL (yellow)
1-30 MeV image and 100 keV /1-30 MeV lightcurves1-30 MeV image and 100 keV /1-30 MeV lightcurves
The EUV/radio sun.The EUV/radio sun.
Flare in EUV 171 Å pass bandFlare in EUV 171 Å pass band Flare in radioFlare in radio
OutlineOutline
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•A suggestion by J. Starck
•Some other problems.
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•A suggestion by J. Starck
•Some other problems.
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From the photosphere to the corona.From the photosphere to the corona.
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The visible sun.The visible sun.
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Sunspot evolution.Sunspot evolution.
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Swedish Vacuum Telescope.Swedish Vacuum Telescope.
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Solar flare quake.Solar flare quake.
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Solar oscillations.Solar oscillations.
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Oscillations in the MDI high-res. f.o.v.Oscillations in the MDI high-res. f.o.v.
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Helioseismology.Helioseismology.
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Sub-surface structure.Sub-surface structure.
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Backside imaging.Backside imaging.
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Longitudinal Magnetic fieldLongitudinal Magnetic field
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304 Å Sun304 Å Sun
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195 Å Sun195 Å Sun
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195 Å difference image of an EIT wave195 Å difference image of an EIT wave
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Solar flare in UV cont. and 2 EUV passbands seen by TRACESolar flare in UV cont. and 2 EUV passbands seen by TRACE
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Filament eruptions in TRACE 171 Å passbandFilament eruptions in TRACE 171 Å passband
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Magnetic loops in TRACE 171 Å passbandMagnetic loops in TRACE 171 Å passband
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A flare in TRACE 1600 Å cont. and 171 Å pass bandA flare in TRACE 1600 Å cont. and 171 Å pass band
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Solar tornados Solar tornados
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Largest flare ever recorded in 171 Å pass band.Largest flare ever recorded in 171 Å pass band.
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The outer corona seen in white-light by LASCO C2
2-15 solar radii
The outer corona seen in white-light by LASCO C2
2-15 solar radii
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LASCO C3 7-30 solar radiiLASCO C3 7-30 solar radii
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Active sun seen in LASCO C3Active sun seen in LASCO C3
OutlineOutline
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
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are needed to see this picture.
TRACE 195 ATRACE 195 A
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Images at the time of the first brightening in the
TRACE movie. (Gallagher 2003)
Images at the time of the first brightening in the
TRACE movie. (Gallagher 2003)
Top panels: TRACE 195 Å difference images created by
subtracting each image from a frame taken at 00:42:30 UT.
Bottom panels: LASCO C2 and C3 images showing the similar morphology of the eruption as it propagates away from the
solar surface. (Gallagher 2003)
Top panels: TRACE 195 Å difference images created by
subtracting each image from a frame taken at 00:42:30 UT.
Bottom panels: LASCO C2 and C3 images showing the similar morphology of the eruption as it propagates away from the
solar surface. (Gallagher 2003)
A Standard AnalysisA Standard Analysis
OutlineOutline
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
scale = 2scale = 2
scale = 4scale = 4
scale = 8scale = 8
scale = 16scale = 16
•The top image shows the 30 multiscale edges at scale 8 (green) and 16 (red) over the image at 00:46:34 UT.
•The bottom images zoom in on the fronts.
•The top image shows the 30 multiscale edges at scale 8 (green) and 16 (red) over the image at 00:46:34 UT.
•The bottom images zoom in on the fronts.
A set of edges from 00:46:34 UT to 01:01:58 UT at 2 scalesA set of edges from 00:46:34 UT to 01:01:58 UT at 2 scales
Following a front in TRACE.
Following a front in TRACE.
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OutlineOutline
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
•My motivations - where I got interested in multiscale methods.
•A gallery of data.
•A standard analysis - that surprised me.
•My approach - an attempt at something better.
•Some other problems.
high-energy solar flare imaging
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Sunspot Classification
Multifractal measure ?Shapelets ?
EIT Calibrationcalibration lamp for flat field and filter grid.
Wavelets, Ridgelets, and Curvelets representation?
EIT 284 Å images
Cosmic Rays,Bright Points,Coronal Holes.
Large increase in data volume.
Large increase in data volume.
• 1 passband x 136 images x (1 Mb) = 136 Mb
• 4 passbands x 1440 images x (16.6 Mbs) = 95.6 Gbs
• 1 passband x 136 images x (1 Mb) = 136 Mb
• 4 passbands x 1440 images x (16.6 Mbs) = 95.6 Gbs
Data from just EUV imaging
Data from the entire spacecraft increases from ~1 Gbyte/day to
~1 Tbyte/day
The sun in STEREOThe sun in STEREO
Tomography in space, reconstructing a 3-D view with two spacecraft