Recent Events Reported by Observers

Detected by Jakub Prchlik, Submitted at 2016-08-03T19:44:48

2014-02-19T19:39:46 --> 2014-02-19T20:45:33

The observation covers a section of a prominence (visible in 1330 A and 1400 A). The prominence remains intact throughout the observation and does not change much in intensity. The same prominence is also observed with roll angles of 0 and -45 (starting at 16:27 and 18:07, respectively).

Detected by Jakub Prchlik, Submitted at 2016-08-03T19:40:38

2014-02-19T16:27:46 --> 2014-02-19T17:35:27

The observation covers a section of a prominence (visible in 1330 A and 1400 A). The prominence remains intact throughout the observation and does not change much in intensity. The same prominence is also observed with roll angles of -45 and -90 (starting at 18:07 and 19:39, respectively).

Detected by Milan Gosic, Submitted at 2016-08-03T18:19:59

2016-07-21T17:01:48 --> 2016-07-21T17:25:02

This C1.2 class flare occurred on 21-Jul-2016 at 17:01 in AR12567. The slit crosses the flare. The movie also shows three B flares that happened afterward in the same flaring region.

Detected by Milan Gosic, Submitted at 2016-08-03T18:04:02

2016-07-22T20:05:38 --> 2016-07-22T20:40:27

C2.4 class flare occurred on 22-Jul-2016 IRIS. It starts at 20:05 UT in AR12567. The slit crosses the upper part of the flaring region.

Detected by Milan Gosic, Submitted at 2016-08-03T17:44:06

2016-07-23T01:47:02 --> 2016-07-23T02:09:01

On 23-Jul-2016 IRIS captured an M5.0 class flare. The flare starts at 01:47 UT between AR12567 and AR12565. It is visible in the upper right part of the movie. The slit crosses only a small portion of the flaring region.

Detected by Jakub Prchlik, Submitted at 2016-08-03T15:58:50

2014-03-14T13:42:46 --> 2014-03-14T15:05:37

A persisting coronal rain intensifies during the observation (visible at 1400 A and 2796 A). As the intensity increases, the coronal rain formation height increases. In addition to the main coronal rain, a single coronal rain filament forms approximately twice as high above the surface as the main coronal rain event.

Detected by Jakub Prchlik, Submitted at 2016-08-03T15:37:35

2014-03-14T11:39:46 --> 2014-03-14T13:27:39

The exposure begins with an intense coronal rain event (visible in 1400 A and 2796 A), which crosses the slit. Once the intense rain subsides, coronal rain streams develop at larger radii than the initial event. Initially, the secondary coronal rain develops above the slit, but it eventually falls and crosses the slit.

Detected by Jakub Prchlik, Submitted at 2016-08-02T21:14:04

2014-11-13T11:48:47 --> 2014-11-13T12:43:38

Prominence on the limb encompasses most of the image in 2796 A, however, the structure is not as dominating in 1400 A.

Detected by Jakub Prchlik, Submitted at 2016-08-02T20:52:56

2014-11-13T17:17:25 --> 2014-11-13T17:35:08

The most obvious feature is a strong coronal jet at the image's bottom right. However, a repeating small jet feeds coronal rain at the top right.

Detected by Jakub Prchlik, Submitted at 2016-08-02T20:42:52

2014-11-14T12:12:30 --> 2014-11-14T13:06:14

Coronal rain condenses in a filament near the center of the image and in the top center. The top central rain presides over an active region. The active region produces several jets of material near the solar surface. These jets clearly heat some of the material attempting to condense, which causes some of the previously condensing material to accelerate away from the surface.

Detected by Jakub Prchlik, Submitted at 2016-08-02T20:28:18

2014-11-15T02:50:30 --> 2014-11-15T03:44:14

Coronal rain intensifies throughout the exposure. In the beginning two filaments bring a steady material flow, however, at 03:30:17 more filaments condense from the same location in the corona. The slit scans across the new filaments' origin.

Detected by Jakub Prchlik, Submitted at 2016-08-02T20:03:56

2014-11-15T12:35:26 --> 2014-11-15T13:28:04

Both 1330 A and 2796 A show a prominence. The prominence remains intact and does not evolve much during the observation.

Detected by Jakub Prchlik, Submitted at 2016-08-02T19:30:14

2014-11-17T11:44:09 --> 2014-11-17T12:46:11

The slit spatially scans a peacock tail with high cadence. The peacock tail displays higher contrast with respect to the background in 1330 A than 2796 A. However, 2796 A shows sunspot oscillations at the bottom of the image, which are barely visible at 1330 A.

Detected by Jakub Prchlik, Submitted at 2016-08-02T17:39:55

2014-11-16T15:25:28 --> 2014-11-16T15:34:12

All observed wavelengths (1330, 1400, and 2796 A) show a low intensity flare (unclassified) emanating below a sunspot. The flare creates a closed loop with three terminal ribbon structures inside. The interior ribbon structures dissipate when material ejects from the flare. The slit crosses the event 1 frame after peak intensity.

Detected by Jakub Prchlik, Submitted at 2016-08-02T14:53:50

2014-11-18T01:30:27 --> 2014-11-18T01:42:41

A low intensity flare (visible in 1330 A and 2796 A) creates a secondary lower intensity flare. The secondary flare forms a linear ribbon, while the main flare creates a network of branches from a single flare ribbon. Meanwhile, the coronal hole at the bottom of the image oscillates (easily visible in 2796 A).

Detected by Jakub Prchlik, Submitted at 2016-08-02T14:40:18

2014-11-12T08:46:07 --> 2014-11-12T08:57:39

Two brightening events precede a GOES C1.9 flare (the flare is visible in 1330, 1400, and 2796 A). The flare originates from a single structure, which has three branches at the bottom of the image.

Detected by Jakub Prchlik, Submitted at 2016-08-02T14:16:34

2014-11-12T16:47:50 --> 2014-11-12T16:58:20

A series of explosive events are visible at 1330, 1400, and 2796 A between a set of coronal holes. The brightest event activates first, while the second and third events have a similar intensity. Both the second and third events cross the slit at their respective maximum intensities.

Detected by Jakub Prchlik, Submitted at 2016-08-02T13:51:38

2014-11-10T23:54:16 --> 2014-11-11T00:10:29

All observed wavelengths display a two ribbon flare with a GOES class of C5.4. One ribbon (top) forms a linear structure, while the other ribbon (bottom) forms a closed loop. Following the peak intensity, the closed loop ribbon ejects material. The ejected material crosses the slit and returns as coronal rain (the return is visible only in 1330 A and 1400 A), again crossing the slit.

Detected by Jakub Prchlik, Submitted at 2016-08-01T21:00:42

2014-06-22T12:56:46 --> 2014-06-22T13:25:22

A flare visible in all observed wavelengths (1330, 1400, and 2796 A) occurs in the upper left corner of the observation. GOES classifies the flare as a B7.9 flare. As the flare reaches maximum intensity one of the ribbons crosses the slit. The slit also records waves of absorption visible in the image during the flare's peak intensity. The absorption waves significantly affect emission line profiles. The line profile evolution is most noticeable in Mg II h/k lines.

Detected by Jakub Prchlik, Submitted at 2016-08-01T20:41:38

2014-06-21T19:15:27 --> 2014-06-21T20:22:09

A GOES 1.0 flare visible in 1330, 1400, and 2796 A contains three primary ribbons of flux. One ribbon is stationary. However, the other two ribbons move after splitting from a common ribbon. After separating from one another, the two ribbons pivot about the end away from the break (i.e., the right ribbon rotates about its right end and the left ribbon rotates about its left end.). The fanning ribbons rotate away from one another (both rotate clockwise) after the break. Eventually, the upper fan rotates into the stationary ribbon causing both ribbons to fade.