solar image processing: a multiscale view c. alex young nasa/gsfc c. alex young nasa/gsfc ucla -...

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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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