Recent Events Reported by Observers

Detected by halocme, Submitted at 2017-05-07T05:40:49

2017-05-01T12:55:13 --> 2017-05-01T13:50:25

This eruption was associated with a B3.0 flare from the same region (without NOAA AR number) as the earlier B9.9 flare. The eruption itself was weaker, but the coronal wave is clearly seen to propagate counterclockwise along the limb in difference images especially in 193 A channel.

Detected by halocme, Submitted at 2017-05-07T04:40:48

2017-05-01T03:50:25 --> 2017-05-01T04:30:01

The eruption associated with the B9.9 flare was pronounced in the radial direction. But difference images also show a large scale wave propagating counterclockwise along the limb.

Detected by halocme, Submitted at 2017-05-07T04:40:48

2017-05-01T03:50:25 --> 2017-05-01T04:30:01

The eruption associated with the B9.9 flare was pronounced in the radial direction. But difference images also show a large scale wave propagating counterclockwise along the limb.

Detected by halocme, Submitted at 2017-05-07T01:41:02

2017-05-01T03:45:01 --> 2017-05-01T05:45:01

This eruption came from the same region as the jet on 30 April 2017 18:30 as reported earlier. It now involved ejection of cool material, most of which seemed to fall back. It was associated with a short-duration B9.9 flare.

Detected by halocme, Submitted at 2017-05-07T00:08:11

2017-04-30T18:15:01 --> 2017-04-30T19:15:01

This jet is not clear close to the origin, although small post flare loops are seen indicating magnetic reconnection between closed and open field lines. It is easier to be seen at higher altitudes (within AIA FOV) as the surrounding structures being pushed away. Running difference images (not shown here) reveal an outward motion in intensity deficit (dimming) in all the three channels in the movie.

Detected by halocme, Submitted at 2017-05-06T20:40:51

2017-04-29T22:40:13 --> 2017-04-30T05:00:13

The eruption started slowly in AR 12653 (without a clear filament as a marker) but produced significant coronal dimming on both sides of the flare ribbons. Post eruption arcades were formed, explaining the associated B3.0 long-decay event in soft X-rays. This eruption did not arrive at Earth.

Detected by halocme, Submitted at 2017-05-06T20:40:50

2017-04-29T22:40:13 --> 2017-04-30T05:00:13

The eruption started slowly in AR 12653 (without a clear filament as a marker) but produced significant coronal dimming on both sides of the flare ribbons. Post eruption arcades were formed, explaining the associated B3.0 long-decay event in soft X-rays. This eruption did not arrive at Earth.

Detected by halocme, Submitted at 2017-05-06T20:40:50

2017-04-29T22:40:13 --> 2017-04-30T05:00:13

The eruption started slowly in AR 12653 (without a clear filament as a marker) but produced significant coronal dimming on both sides of the flare ribbons. Post eruption arcades were formed, explaining the associated B3.0 long-decay event in soft X-rays. This eruption did not arrive at Earth.

Detected by halocme, Submitted at 2017-05-06T19:56:37

2017-04-29T12:50:25 --> 2017-04-29T14:40:25

This may be a disk view of a failed eruption which does not escape from the Sun. It occurred in AR 12653, which had already decayed to 1/3 of its maximum size.

Detected by halocme, Submitted at 2017-05-06T19:48:25

2017-04-28T14:00:09 --> 2017-04-28T17:30:09

The eruption nicely shows helical motions that may indicate a flux rope. Some citizen scientists said that this was a breakout eruption, but it does not look that way. Reconnection signatures expected before and during the main eruption are weak. This may be more consistent with kink- or torus-unstable eruption. The eruption in the radial direction was obviously not smooth with disturbances slowly moving horizontally, especially counterclockwise. This is consistent with disappointingly small presence of the consequence of the eruption in LASCO data.

Detected by halocme, Submitted at 2017-05-06T19:34:03

2017-04-28T13:55:13 --> 2017-04-28T15:01:13

At low temperatures, this event looks like a mini filament (prominence) eruption, but in 211 A channel (especially in running difference images, not shown here) it is more like a jet. Perhaps another example to suggest the intimacy between these two phenomena.

Detected by halocme, Submitted at 2017-05-06T19:34:03

2017-04-28T13:55:13 --> 2017-04-28T15:01:13

At low temperatures, this event looks like a mini filament (prominence) eruption, but in 211 A channel (especially in running difference images, not shown here) it is more like a jet. Perhaps another example to suggest the intimacy between these two phenomena.

Detected by halocme, Submitted at 2017-05-06T19:25:33

2017-04-27T00:10:13 --> 2017-04-27T01:00:13

One jet close to the limb was followed by another with clearer footpoint brightening. These may be nothing special, but they are more easily discernible than others.

Detected by Jean-Pierre Wuelser, Submitted at 2017-05-04T22:06:46

2017-04-29T07:43:36 --> 2017-04-29T08:36:07

Small (recurring) surge

Detected by Jean-Pierre Wuelser, Submitted at 2017-05-04T21:47:27

2017-04-26T15:35:35 --> 2017-04-26T17:34:44

Filament activation followed by a very small two-ribbon flare

Detected by Peter Levens, Submitted at 2017-05-01T15:14:37

2017-04-02T03:50:02 --> 2017-04-02T07:43:46

This large prominence was seen at the south-west solar limb over a number of days. It is very dynamic, with apparent flows in all directions. This study has long exposure times in order to enhance the C II and Si IV lines that are visible in emission in prominences, but are much weaker than the Mg II lines. At around 05:30 UT a brighter flow feature appears from the solar disc and interacts with the prominence magnetic field.

Detected by Peter Levens, Submitted at 2017-05-01T15:05:49

2017-03-31T22:50:58 --> 2017-03-31T23:36:32

A low-C class flare can be seen in this sit-and-stare movie, peaking at around 22:58 UT. The curved flare ribbon is seen to cross the slit in the east-west direction.

Detected by Peter Levens, Submitted at 2017-05-01T14:53:01

2017-03-30T07:08:03 --> 2017-03-30T08:48:33

This quiescent prominence at the NW limb was observed with IRIS in coordination with SUMER. Despite being a quiescent prominence a number of flows can be seen, where cool material traces dips in the magnetic field embedded in the hot solar corona.

Detected by Peter Levens, Submitted at 2017-05-01T14:46:14

2017-03-28T04:13:11 --> 2017-03-28T05:04:20

A 'peacock tail' was seen by IRIS above a sunspot in AR 12644. This study was designed as a large AR monitoring study so the slit only crossed the peacock tail at the start of the raster, however the wavy phenomenon can be seen in the slit-jaw movie after the slit has moved past it.

Detected by Peter Levens, Submitted at 2017-05-01T14:35:20

2017-03-29T16:28:17 --> 2017-03-29T17:02:39

During an AR monitoring study on AR 12644 a partial eruption occurred as the IRIS slit crossed this region. Seeming to originate at a bright point, material emerges into the solar atmosphere but is mostly contained by the magnetic field. It then flows in both directions along the magnetic field loops above.