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Solar Image Processing: A Multiscale View C. Alex Young NASA/GSFC C. Alex Young NASA/GSFC UCLA - IPAM (January 28, 2004)

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Presentation on theme: "Solar Image Processing: A Multiscale View C. Alex Young NASA/GSFC C. Alex Young NASA/GSFC UCLA - IPAM (January 28, 2004)"— Presentation transcript:

1 Solar Image Processing: A Multiscale View C. Alex Young NASA/GSFC C. Alex Young NASA/GSFC UCLA - IPAM (January 28, 2004)

2 Outline 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.

3 Outline 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.

4 The high energy sun. 20 Jan 2000 Solar Flare BATSE and COMPTEL (yellow) 1-30 MeV image and 100 keV /1-30 MeV lightcurves

5 The EUV/radio sun. Flare in EUV 171 Å pass band Flare in radio

6 Outline 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.

7 From the photosphere to the corona.

8 The visible sun.

9 Sunspot evolution.

10 Swedish Vacuum Telescope.

11

12 Solar flare quake.

13 Solar oscillations.

14 Oscillations in the MDI high-res. f.o.v.

15 Helioseismology.

16 Sub-surface structure.

17 Backside imaging.

18 Longitudinal Magnetic field

19

20 304 Å Sun

21

22

23

24 195 Å Sun

25

26 195 Å difference image of an EIT wave

27 Solar flare in UV cont. and 2 EUV passbands seen by TRACE

28 Filament eruptions in TRACE 171 Å passband

29 Magnetic loops in TRACE 171 Å passband

30 A flare in TRACE 1600 Å cont. and 171 Å pass band

31 Solar tornados

32 Largest flare ever recorded in 171 Å pass band.

33

34 The outer corona seen in white-light by LASCO C solar radii The outer corona seen in white-light by LASCO C solar radii

35 LASCO C solar radii

36 Active sun seen in LASCO C3

37 Outline 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.

38 TRACE 195 A

39

40 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)

41 A Standard Analysis

42 Outline 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.

43 scale = 2 scale = 4 scale = 8 scale = 16

44 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 scales

45 Following a front in TRACE.

46 Outline 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.

47 high-energy solar flare imaging

48

49 Sunspot Classification Multifractal measure ? Shapelets ?

50 EIT Calibration calibration lamp for flat field and filter grid. Wavelets, Ridgelets, and Curvelets representation?

51 EIT 284 Å images Cosmic Rays, Bright Points, Coronal Holes.

52 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

53 The sun in STEREO Tomography in space, reconstructing a 3-D view with two spacecraft


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