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Finding which solar events made it to interplanetary space

Finding which solar events made it to interplanetary space. Nariaki Nitta (LMSAL). It is important to compare jmaps with movies of images.

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Finding which solar events made it to interplanetary space

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  1. Finding which solar events made it to interplanetary space Nariaki Nitta (LMSAL)

  2. It is important to compare jmaps with movies of images • It is hard to quantify what you see in movies. If we end up measuring some features, we will be typically stuck at one or a limited number of position angles ---> jmaps • Jmaps at one position angle may miss lots of things, such as non-radial motions and motions observed only for limited distances, so examining movies is also important. Alternatively, one can also study jmaps at different position angles, even though only the features that are ecliptic matter for comparisons with in-situ data. • Of course we should remember the motions seen in images are projected on to the plane of the sky. • Also, the artifact of running difference images (Harrison)?

  3. Jmaps between PA 70 and PA 100, using Jackie Davies’ software(PA85 = ecliptic)

  4. It appears that only two tracks made it to 1 AU (indicated by the long arrows). Are they “L”, and “A” or “B”? • Their origins in COR2, as I had thought before the trip, are indicated by the short arrows. But this may be easily challenged.. • There seems to be no way the earlier events (e.g., on 30-Jul-2010) contributed to the in-situ signatures after 3-Aug-2010.

  5. Five COR2-A CMEs on 1 August 2010 04:08 09:08 10:08 Initially, I had thought that the two CMEs framed in red were responsible for the HI and in-situ signatures, but the second one may be questioned. 17:08 22:08

  6. Automated CME detection CACTus (http://secchi.nrl.navy.mil/cactus/) output The CME around 16-17 UT is missing.

  7. Five COR1-A CMEs on 1 August 2010 03:00 07:47 08:50 16:30 20:50

  8. COR1-A Movie / http://www.lmsal.com/nitta/movies/flares_euvi/FESTIVAL_QT_MOVIES/20100801_00_a_cor1_raw_euvi195_diff.mov

  9. Movies of AIA and EUVI Running Difference Images CME2 associated with the C3 flare at AR 11192 AIA EUVI-A Filament1, which started to slowly rise around 5 UT, did not erupt yet. http://www.lmsal.com/nitta/science/20100801_eruptions/aia_euvia_rdiff_20100801_0730.mov

  10. Movies of AIA and EUVI Running Difference Images CME4 from a quiescent region southwest of Filament1 AIA EUVI-A Can such a small eruption from a western region get out to the heliosphere? Maybe this was the “B” track not arriving at 1 AU? http://www.lmsal.com/nitta/science/20100801_eruptions/aia_euvia_rdiff_20100801_1530.mov

  11. Flux rope modeling This just illustrates how the fitting works for CME2. We need to do this more systematically for CME3 and CME4 at different times . But beware of the limitation when the CME does not have a smooth leading edge.

  12. COR1-A, COR2-A Movie for CME3 It was discussed that the second ICME (presumably corresponding to HI track A) may have been related to CME3 (the eruption of filament1), which appears to be complex. Is it possible that what looks like an internal structure results in a flux rope at 1 AU? http://www.lmsal.com/nitta/science/20100801_eruptions/cor1cor2_20100801.mov

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