Recent Events Reported by Observers

Detected by halocme, Submitted at 2012-09-29T05:06:53

2012-09-24T04:50:23 --> 2012-09-24T06:00:23

This may serve as an example of eruption that starts at relatively high altitudes without much flaring lower down - no flare above the background ~B5 level.

Detected by halocme, Submitted at 2012-09-29T05:00:40

2012-09-24T02:10:11 --> 2012-09-24T03:10:11

The motion appears to be largely radial.

Detected by anny, Submitted at 2012-09-29T03:27:02

2012-09-27T21:00:03 --> 2012-09-28T02:56:03

The highlighted bundle of coronal loops appears to be relatively short and therefore possibly overlying a flux rope. Peculiarly, they do not appear to be affected at all by the eruption

Detected by anny, Submitted at 2012-09-29T03:24:20

2012-09-27T21:00:03 --> 2012-09-28T02:56:03

Soon after sigmoid eruption.

Detected by anny, Submitted at 2012-09-29T03:07:56

2012-09-27T21:28:03 --> 2012-09-28T01:42:03

Eruption of a beautiful sigmoid on the W disk and the following postflare arcade.

Detected by anny, Submitted at 2012-09-29T03:07:56

2012-09-27T21:28:03 --> 2012-09-28T01:42:03

Eruption of a beautiful sigmoid on the W disk and the following postflare arcade.

Detected by halocme, Submitted at 2012-09-29T00:19:15

2012-09-23T14:00:07 --> 2012-09-24T00:00:07

The eruption itself seems to be not very spectacular (not associated with abig CME), but the post-flare loops are quite perstent. The source region seems to be just over the limb. This temporally follows the big eruption at E110, but their relation is not clear.

Detected by halocme, Submitted at 2012-09-28T22:59:45

2012-09-23T20:30:35 --> 2012-09-23T21:30:35

This is a small eruption, but it affects the areas not only in the radial direction but also in lateral directions. For example, loops to the west, seen at 171 A in particular, seem to oscillate in association with the eruption, which should be understood in 3-d.

Detected by halocme, Submitted at 2012-09-28T22:27:38

2012-09-23T02:50:23 --> 2012-09-23T03:40:23

Better viewed in running difference images, a thin structure slightly brightens up for short time. This is probably a jet.

Detected by halocme, Submitted at 2012-09-28T21:57:52

2012-09-23T03:00:03 --> 2012-09-23T05:00:03

Expanding loops seem to leave mild coronal dimming and ribbons of bright areas as in more energetic eruptions. There is an indication that these expanding loops also affect the larger-scale filament to southweat.

Detected by halocme, Submitted at 2012-09-28T20:32:21

2012-09-22T20:30:35 --> 2012-09-22T21:59:23

This eruption seems to be better viewed in the form of running difference movies. This follows or is closely related with the" eruptions supoerposed?" as reported earlier. The driver seems to reside in souther regions, but the body of the eruption is in the northern hemisphere.

Detected by halocme, Submitted at 2012-09-28T20:07:50

2012-09-22T16:30:35 --> 2012-09-22T21:02:35

It seems that the filament eruption in the southern region, which seems to be more horizontal than vertical, helps prominence to the north to erupt and become unstable.

Detected by halocme, Submitted at 2012-09-28T18:55:13

2012-09-22T13:30:35 --> 2012-09-22T15:00:35

The associated brightening, although minor, is quite clear. It is not only the two ribbon close to the surface, but is seen at some altitudes for shorter time.

Detected by halocme, Submitted at 2012-09-28T18:32:17

2012-09-22T12:15:35 --> 2012-09-22T13:15:35

A very minor eruption seen most clearly at 171 A seems to have some impact on higher altitudes.

Detected by halocme, Submitted at 2012-09-28T17:23:09

2012-09-22T19:00:04 --> 2012-09-22T23:00:04

Selected this time range on the basis of a DH radio spectrum from Wind WAVES. Two type III bursts are seen around 20 UT and 21 UT. STEREO-B data show two regions around S15 E98 and S15 E125 participate in activity. It appears that the post-flare loops (responsible for the GOES B9.2 flare starting at 19:30) seen in 94 A images come from the region closer to the limb, although the type III burst lacks high frequency component, often considered to come from a region deeply occulted. Another region was also involved in two eruptions corresponding to the radio bursts.

Detected by halocme, Submitted at 2012-09-27T04:45:22

2012-09-23T13:50:23 --> 2012-09-23T16:59:59

The region that produced a big flare and eruption on 20-Sep-2012 is now at S15 E110, only 20 degrees behind the limb. This event may be not as dramatic as the one on September 20, but EUVI data show more large-scale structures away from the active region participate in the eruption. Accordingly the flare time profile is more gradual.

Detected by halocme, Submitted at 2012-09-26T23:02:47

2012-09-22T02:40:11 --> 2012-09-22T03:19:47

This may not be as specacular as the one on September 20, but it is observed as a partial halo CME. The source region is S15 E135.

Detected by halocme, Submitted at 2012-09-25T18:50:36

2012-09-20T14:50:23 --> 2012-09-20T15:31:11

STEREO-B EUVI data show an intense flare at S15 E153 (from Earth). The occultation height at this longitude is almost 0.8Rs. The flare magnitude could be X10 on the basis of EUVI data. The EUV wave signature is quite modest. COR1A data indicate that the CME was initially as fast as 3500 km/s (according to my back-of-envelop calculation).

Detected by halocme, Submitted at 2012-09-25T15:59:20

2012-09-21T11:50:23 --> 2012-09-21T13:00:23

A filament can deform as it erupts. Only after these motions, does the wetern part seem to erupt. In a more global picture, the eruption that directly drives a CME may have already taken place before 1200 UT, and the part of the filament that attracts our eyes may be just internal structures.

Detected by halocme, Submitted at 2012-09-25T15:05:36

2012-09-21T01:20:23 --> 2012-09-21T02:20:23

This may be a kind of coronal jet although as dimming. It is not as readily visible at 171 A or 211 A.