17 December 2017

Movie Gallery

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Coronal Mass Ejections


|9603c1ro | 9605c1ro | 9606c1sm | 960708c1 | 9608c1c2 | 961018c1 | c3_2year | fastSW | Xmas99 | May2kv3 |
9603c1ro

The inner corona in March 1996, a time period of extremely low solar activity,observed by LASCO-C1 at  a  wave  length  of   530.3 nm. The  continuum intensity  at 530.9 nm  was subtracted from   each image.The residual intensity made visible this way is emitted from coronal Fe-XIV ions at a temperature of 1.5 million degrees. There are 10 images/day with data   gaps interpolated  accordingly (seconds marked as ":01"). The images are not calibrated by suitable flatfield images.A scientific discussion of this movie can be found in the publication by Schwenn et al. in Solar Physics special issue II (1997).
29.2.1996 21:35 - 18.3.1996 19:11
181 frames, 512x512, 45.27MB (MVI),  source: MPS
9605c1ro

The inner corona during two solar rotations in summer 1996, a time period of low solar activity, observed by LASCO-C1  at a  wave  length of 530.3nm. The continuum intensity at 530.9 nm was subtracted  from each  image. The   residual  intensity   made  visible  this  way   is emitted  from  coronal  Fe-XIV  ions  at  a temperature of 1.5 million degrees. There are  10 images/day  with data gaps interpolated  accordingly  (seconds marked as ":01"). In  the center  of the images, the  strength of the  photospheric  magnetic   field  is  displayed  in a color code (light  green: positive field  directed away from the  Sun, dark  green:  negative   field, directed towards  the  Sun,  the  solid line represents   the  magnetic  neutral line). The photospheric  magnetic  field data were  kindly  supplied  from  the Wilcox Solar Observatory, Stanford, USA.
15.5.1996 00:00 - 19.7.1996 14:24
657 frames, 416x280, 73.06MB (MVI), 10.41MB (MPEG), source: MPS
9606c1sm

A sequence of CMEs above the western limb of the Sun in  June 1996, observed by LASCO-C1 at a wave length of 530.3 nm. The continuum intensity at 530.9nm was subtracted from each image. The residual intensity made visible this way is emitted from coronal Fe-XIV ions at a temperature of 1.5 million degrees.The time between two consecutive image varies al little and is rougly 45min.In the center of the images, the strength of the photospheric magnetic field is displayed in a color code (light green: positive field directed away from the Sun, dark green: negative field, directed towards the Sun, the solid line  represents the magnetic neutral line). The photospheric magnetic field data were kindly supplied from the Wilcox Solar Observatory, Stanford, USA.
13.6.1996 12:00 - 24.6.1996 00:00
351 frames, 360x400, 48.25MB (MVI), 10.26MB (MPEG),   source: MPS
960708c1

A slow mass ejection from the corona observed by LASCO-C1 at  a wave length of 530.3 nm. The continuum intensity at 530.9 nm  was subtracted  from each image. The residual intensity made visible this way is emitted from coronal Fe-XIV ions  at a  temperature of 1.5 million  degrees. The images  are not calibrated by  flat field images, pixel defects by cosmic ray hits have  no yet been removed.
8.7.1996 04:39 - 8.7.1996 14:26
15 frames,  388x388,  2.15MB (MVI), 0.66MB (MPEG),   source: MPS
961018c1

Two CMEs observed  by LASCO-C1 at a wave length of 530.3 nm. The   continuum intensity at 530.9 nm was subtracted from each image.The residual intensity made visible this way is emitted from coronal Fe-XIV  ions at a temperature of 1.5 million degrees. The images are not calibrated  by flat field images,pixel defects by cosmic ray hits have not yet been removed.
18.10.1996 02:25 - 19.10.1996 23:03
46 frames, 419x544, 10.01MB (MVI), 2.30MB (MPEG),   source: MPS
9608c1c2

The solar corona during the  'Whole Sun Month'  (10. Aug.  -  8. Sep. 1996),observed by  LASCO-C1 at a wave length of 530.3nm  and by LASCO-C2 in white light.In the center of the images, the strength of the photospheric magnetic field is displayed in a color code  (red:  positive field directed away from  the Sun,  blue:  negative field,  directed towards the Sun). The photospheric magnetic field data were kindly supplied from the Wilcox Solar Observatory, Stanford, USA.
12.8.1996 23:02 - 8.9.1996 07:20
138 frames, 512x288, 2.75MB (MPEG), source: MPS
c3_2year
1.5.1996 00:39 - 4.5.1998 01:44

2848 frames, 512x512, 96.08MB (MPEG), source: NRL
fastSW

244 frames, 320x240, 2.31MB (MPEG)
Xmas99
15.12.1999 00:42 - 06.01.2000 23:42
529 frames, 720x576, 28.00MB (MPEG)