Recent Events Reported by Observers

Detected by Jakub Prchlik, Submitted at 2016-08-05T16:08:05

2014-07-30T00:23:53 --> 2014-07-30T00:59:08

IRIS captures a GOES class C1.3 flare in AR 12125 (visible in 1330 Å and 2796 Å). The flare starts as a small bright ribbon slightly right of center. The ribbon remains bright for a few frames until a bright region emerges to its left. Soon after the bright region emerges the ribbon quickly expands to the left. Once the ribbon ceases moving left, the flare expands to the right. The expansion registers as blueshifted and redshifted emission in common lines (e.g., Mg II h/k).

Detected by Jakub Prchlik, Submitted at 2016-08-05T15:39:19

2014-08-01T17:54:59 --> 2014-08-01T18:54:29

IRIS observes a GOES class M1.5 flare, which is visible in 1330, 1400, and 2796 Å. The flare originates in two ribbons near the image's center. After formation, the ribbons move away from each other and decrease in intensity. The top ribbon stalls over a coronal hole and leaves behind a heated filament.

Detected by Jakub Prchlik, Submitted at 2016-08-05T14:56:55

2014-08-04T15:37:41 --> 2014-08-04T15:47:54

IRIS in coordination with SUMER observes an unclassified flare in the image's upper right (marked). The flare forms via two roughly circular bright regions near the edge of a filament. Another flare forms later in the observation in the bottom eighth of the image and crosses the slit. However, most of the flare is outside the image. This flare creates a coronal rain, which extends to the position of the marked flare.

Detected by Jakub Prchlik, Submitted at 2016-08-05T14:37:58

2014-08-03T14:44:31 --> 2014-08-03T15:06:52

A series of low intensity flares (no GOES classification) arise during a coordinated observation with SUMER. The flares (visible in 1400 Å and 2796 Å) primarily occur on the boundary of three nearby coronal holes located slightly left of center. The brightest, most interesting flare (marked) weaves around the three coronal holes. The slit captures a brightening region associated with this flare.

Detected by Jakub Prchlik, Submitted at 2016-08-05T14:15:48

2014-08-02T07:53:37 --> 2014-08-02T08:17:34

IRIS (in coordination with SUMER) observes two low intensity flares (the first, more intense flare is marked) in the image's top left corner. Later coronal rain develops over regions where the low flares occurred. An unclassified, off image flare occurring at 09:45 likely initiates the rain. The coronal rain crosses the slit, however, the spectroscopic observations do not show any interesting features.

Detected by Jakub Prchlik, Submitted at 2016-08-04T21:15:22

2014-07-30T20:01:33 --> 2014-07-30T22:25:10

All observed wavelengths (1330, 1400, and 2796 Å) display sunspot oscillations in a coordinated observation with BBSO. The oscillations are best visible at 2796 Å and do not cross the slit.

Detected by Jakub Prchlik, Submitted at 2016-08-04T20:57:40

2014-07-29T15:34:43 --> 2014-07-29T15:55:48

A small flare, best visible at 1330 Å but also visible at 2796 Å, occurs during a coordinated observation with VTT/DST. The flare forms a V shape and its vertex crosses the slit. The flare's intensity saturates and broadens the C II and Si IV spectral lines.

Detected by Jakub Prchlik, Submitted at 2016-08-04T19:04:55

2014-05-09T02:20:37 --> 2014-05-09T02:53:54

An unclassified flare on the limb dominates the image of AR 12047 (encompassing the image's entire bottom half). As such, the slit captures the event. The spectral lines oscillate from redshifted to blueshifted in a sinusoidal pattern. The oscillation pattern's wavelength increases as time since the flare increases. As such, the spectrum initially shows one and a half oscillation wavelengths, but decays to less than a wavelength in two frames.

Detected by Jakub Prchlik, Submitted at 2016-08-04T18:36:31

2014-05-08T10:50:44 --> 2014-05-08T15:12:25

An unclassified flare in AR 12060 initiates a down pour of coronal rain. The flare begins by ejecting material into the corona, but the jet subsides approximately 20 frames after maximum extent. Once the material reaches the corona, the corona rapidly responds by creating a network of coronal rain arches. The coronal rain event is short lived, like the jet. Still, the active area, which produced the jet, remains bright for most of the observation and is covered by the slit. When the active area is bright the spectrum shows an increase in emission features (~ a factor of two) and line broadening.

Detected by Jakub Prchlik, Submitted at 2016-08-04T17:58:24

2014-05-12T03:12:24 --> 2014-05-12T03:27:40

IRIS observes part of a GOES C1.3 flare in the image's bottom left. The flare does not cross the slit, however, AR 12058 also creates a secondary low intensity flare (unclassified in GOES). The secondary flare does cross the slit.

Detected by Jakub Prchlik, Submitted at 2016-08-04T17:40:46

2014-05-11T17:07:58 --> 2014-05-11T17:26:30

IRIS observes a GOES C3.1 Flare in AR 12056. The flare originates on either side of a coronal hole in the image's bottom left. In addition, a sunspot on the bottom right shows oscillations in 1330 Å and 2796 Å.

Detected by Jakub Prchlik, Submitted at 2016-08-04T17:25:11

2014-05-10T14:55:52 --> 2014-05-10T15:15:03

A low intensity (no GOES classification) flare encompasses most of the image's upper left. The flare originates from two separate brightening regions, which eventually connect and produce a sigmoid like flare. In addition, the sunspot in the lower right shows two origins for the oscillations, which creates an interference pattern in the oscillations.

Detected by Jakub Prchlik, Submitted at 2016-08-04T17:09:51

2014-05-10T02:28:29 --> 2014-05-10T03:50:08

All observed wavelengths (1330, 1400, and 2796 Å) display sunspots oscillations. The oscillations are most obvious in 2796 Å, however, 2796 Å's oscillations appear more chaotic than the oscillations in 1330 Å and 1400 Å. The observation also captures two small flares. One flare is a simple filament, while the second more intense flare creates a V shape.

Detected by Jakub Prchlik, Submitted at 2016-08-04T16:28:20

2014-05-07T18:01:41 --> 2014-05-07T18:11:28

AR 12055 shows a low intensity flare and a series of brightenings around a coronal hole. Both events broaden spectral lines lines like C II and Si IV and increase the continuum flux.

Detected by Jakub Prchlik, Submitted at 2016-08-04T16:05:25

2014-05-06T06:35:20 --> 2014-05-06T06:49:40

A region crossing slit erupts in three flare events. The flares' intensity is similar for all three eruptions in AR 12051. After each small flare, the coronal rain intensifies.

Detected by Jakub Prchlik, Submitted at 2016-08-04T15:42:31

2014-05-11T06:49:38 --> 2014-05-11T07:08:40

A small eruption occurs during a coordinated LaPalma QS observation. However, only the 1400 Å image shows the eruption. During the eruption, C II lines display a redshifted emission feature.

Detected by Jakub Prchlik, Submitted at 2016-08-04T15:08:11

2014-02-22T17:49:28 --> 2014-02-22T19:00:26

Both 1330 Å and 1400 Å show a stable prominence. The prominence does not change its structure or intensity even when a small eruption occurs approximately half way through the exposure (18:19:42). However, it is not clear whether the eruption and the prominence are spatially coherent (i.e. the small eruption may be in the foreground).

Detected by Jakub Prchlik, Submitted at 2016-08-04T14:54:47

2014-02-20T20:20:03 --> 2014-02-20T21:29:49

All observed wavelengths (1330, 1400, and 2796 Å) show coronal rain over AR 11986. The rain primarily returns to the surface via arches, however, a large material stream enters the image in the last 25 frames (21:11:36).

Detected by Jakub Prchlik, Submitted at 2016-08-03T20:22:34

2014-02-20T02:20:14 --> 2014-02-20T02:30:38

The observation captures two low intensity flares (no GOES classification). The first flare is lower in intensity but larger in extent than the second flare. Both flares occur along the edge of the same coronal hole.

Detected by Jakub Prchlik, Submitted at 2016-08-03T19:48:46

2014-02-19T18:07:46 --> 2014-02-19T19:04:07

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 -90 (starting at 16:27 and 19:39, respectively).