Recent Events Reported by Observers
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Detected by Jacob Parker, Submitted at 2017-04-25T15:59:45
2017-04-13T17:53:37 --> 2017-04-13T19:00:47
A region of changing flux associated with a small flare.
Detected by Jacob Parker, Submitted at 2017-04-25T15:45:51
2017-04-13T14:01:55 --> 2017-04-13T16:33:21
Co-observing spicules at the North Pole
Detected by Jacob Parker, Submitted at 2017-04-25T15:30:03
2017-04-12T16:33:09 --> 2017-04-12T17:25:30
Deep sit-and-stare on portion of micro-flare footpoint
Detected by Jacob Parker, Submitted at 2017-04-25T14:54:30
2017-04-11T11:00:56 --> 2017-04-11T11:21:24
Small flare ribbon observed during hot loops observation.
Detected by Joten Okamoto, Submitted at 2017-04-25T12:13:14
2017-04-18T23:40:44 --> 2017-04-19T03:35:35
We can see two prominence structures along the line of sight. One is a curtain-like faint prominence, and the other one is a dragon-like (?) shape. The dragon cranes his neck to the solar surface, and the plasma flows down.
Detected by Joten Okamoto, Submitted at 2017-04-27T17:13:04
2017-04-22T10:01:24 --> 2017-04-22T10:44:31
An irregular-shaped two-ribbon flare is observed in AR 12651. A faint feature seems to be ejected northward by the explosion, which shows a strong blueshift only in the Si IV line (no Dopplershift in other lines).
Detected by Joten Okamoto, Submitted at 2017-04-25T11:55:39
2017-04-18T20:22:29 --> 2017-04-18T21:23:52
IRIS captured formation of post-flare loops related to a C-class flare in AR 12651 at the east limb.
Detected by Joten Okamoto, Submitted at 2017-04-25T11:44:40
2017-04-23T02:57:55 --> 2017-04-23T03:24:33
A region sandwiched by two umbrae (AR 12651) shows numerous brightenings. A relatively-large brightening, or a small flare with two ribbons, occurs and some plasmas are ejected northward from the active area.
Detected by Joten Okamoto, Submitted at 2017-04-25T05:11:19
2017-04-20T13:22:33 --> 2017-04-20T17:17:41
The off-limb region over AR 12651 presents coronal rains. They flow down along invisible magnetic field lines (coronal loops). After the raining, a small activation takes place in the same region, which looks like a twisting motion. The IRIS slit scans over these phenomena.
Detected by halocme, Submitted at 2017-04-22T10:10:18
2017-04-20T20:30:01 --> 2017-04-20T23:00:01
This seems to be a classic filament eruption, resulting in the formation of separating chromospheric ribbons. It occurred next to a decayed active region without spots. The associated CME was mostly toward north (see http://spaceweather.gmu.edu/seeds/mkmovie.php?cme=20170420.221207.w054.v0227.p369&frame=15&r).
Detected by halocme, Submitted at 2017-04-22T10:03:48
2017-04-20T18:00:09 --> 2017-04-20T22:00:09
A concave structure, probably representing a flux rope, is seen to form above the prominence during the eruption. This is seen most clearly in 171 A channel.
Detected by halocme, Submitted at 2017-04-22T09:56:25
2017-04-20T15:55:13 --> 2017-04-20T17:31:13
This gives an impression that one leg (north) of the filament got loose and erupted. It was located in a quiescent region detached from AR 12651. The eruption was associated with a CME (http://spaceweather.gmu.edu/seeds/mkmovie.php?cme=20170420.171207.w057.v0336.p077&frame=14&r).
Detected by halocme, Submitted at 2017-04-22T10:41:33
2017-04-18T18:55:14 --> 2017-04-19T02:01:14
The flare lasted long, and as expected, was associated with a more decent CME than the previous flare. This one does not show clear coronal waves, and the expansion was more in the radial than horizontal directions. After the peak downward motions are seen from the top of the arcade which is hot. Shortly after the eruption, big motions were seen, but these are image motions. Indeed, the peak of the flare coincided with AIA weekly calibration.
Detected by halocme, Submitted at 2017-04-22T10:41:32
2017-04-18T18:55:14 --> 2017-04-19T02:01:14
The flare lasted long, and as expected, was associated with a more decent CME than the previous flare. This one does not show clear coronal waves, and the expansion was more in the radial than horizontal directions. After the peak downward motions are seen from the top of the arcade which is hot. Shortly after the eruption, big motions were seen, but these are image motions. Indeed, the peak of the flare coincided with AIA weekly calibration.
Detected by halocme, Submitted at 2017-04-22T10:41:32
2017-04-18T18:55:14 --> 2017-04-19T02:01:14
The flare lasted long, and as expected, was associated with a more decent CME than the previous flare. This one does not show clear coronal waves, and the expansion was more in the radial than horizontal directions. After the peak downward motions are seen from the top of the arcade which is hot. Shortly after the eruption, big motions were seen, but these are image motions. Indeed, the peak of the flare coincided with AIA weekly calibration.
Detected by halocme, Submitted at 2017-04-22T09:40:50
2017-04-18T09:20:25 --> 2017-04-18T10:50:25
AR 12644, which produced M-class flares on 1-2 April 2017 came back as AR 12651, producing two C-class flares on 18 April 2017. The first one was associated with a mediocre CME, but it accompanied a coronal wave propagating along the limb (counterclockwise) and into the disk.
Detected by halocme, Submitted at 2017-04-22T09:40:50
2017-04-18T09:20:25 --> 2017-04-18T10:50:25
AR 12644, which produced M-class flares on 1-2 April 2017 came back as AR 12651, producing two C-class flares on 18 April 2017. The first one was associated with a mediocre CME, but it accompanied a coronal wave propagating along the limb (counterclockwise) and into the disk.
Detected by gchintzo, Submitted at 2017-04-21T22:03:41
2017-04-17T18:10:09 --> 2017-04-18T00:00:09
A third occurence of a jet-like CME eruption originating from this source region on the East limb (320km/sec; http://spaceweather.gmu.edu/seeds/mkmovie.php?cme=20170417.222407.w015.v0322.p091&frame=9&r). Same as previously, a confined eruption is followed by a more extended eruption.
Detected by gchintzo, Submitted at 2017-04-21T21:56:57
2017-04-17T10:00:09 --> 2017-04-17T18:00:09
The source region of a jet-like CME observed by LASCO (321 km/sec; http://spaceweather.gmu.edu/seeds/mkmovie.php?cme=20170417.154807.w019.v0321.p090&frame=11&r). Same as in previous entry, a confined filament eruption is followed by an eruption which exceeds AIA's field of view.
Detected by gchintzo, Submitted at 2017-04-21T20:55:08
2017-04-17T05:00:09 --> 2017-04-17T10:50:09
The source region of a jet-like ejection seen in the LASCO observations ( ~400km /sec http://spaceweather.gmu.edu/seeds/mkmovie.php?cme=20170417.080007.w024.v0404.p090&frame=10&r). A jet-like confined eruption is followed by a rapid dimming in the overlying corona suggesting a non-radial eruption. However, the ejection seen in LASCO from this part of the Sun shows a more radial-like jet-like CME.
