Recent Events Reported by Observers

Detected by Hans Courrier, Submitted at 2016-08-09T21:05:47

2016-08-02T21:43:19 --> 2016-08-02T22:55:38

Spicules near quiet sun network element.

Detected by Hans Courrier, Submitted at 2016-08-09T21:03:08

2016-08-02T20:10:19 --> 2016-08-02T21:32:27

Spicules near quiet sun network element.

Detected by Jakub Prchlik, Submitted at 2016-08-09T20:08:47

2014-07-04T23:15:49 --> 2014-07-04T23:37:41

A low intensity flare crosses a sunspot perpendicular to a light bridge. The unclassified flare in AR 12104 forms two roughly parallel ribbons across the sunspot before intensifying.

Detected by Jakub Prchlik, Submitted at 2016-08-09T19:59:37

2014-07-05T23:26:48 --> 2014-07-06T01:48:50

A sunspot near the image's center contains two light bridges (visible in 1330 Å and 2796 Å). The bridge on the right contains a peacock tail, which fades by the observation's end (only visible in 1330 Å).

Detected by Jakub Prchlik, Submitted at 2016-08-09T19:41:30

2014-07-07T11:29:36 --> 2014-07-07T15:10:16

The third spray surge from AR 12114 in a week (previous spray surges occurred on 7/01/2014 and 07/03/2014). This spray surge also repeats in the same observation with the second spray surge ejecting more material than the first spray surge. Still, both spray surges cross the slit and produce higher intensity, velocity shifted lines.

Detected by Jakub Prchlik, Submitted at 2016-08-09T19:30:01

2014-07-03T13:18:02 --> 2014-07-03T14:29:03

A spray surge originates offscreen, but soon encompasses the image's upper third (visible in 1330 Å and 1400 Å). The surge is the second observed in the same region (first observe 2 days prior). Like the previous spray surge observation, this spray surge crosses the slit. The spray surge intensifies common spectral lines, and the surge's motion adds velocity shifted emission components to the lines.

Detected by Jakub Prchlik, Submitted at 2016-08-09T19:11:20

2014-07-01T12:45:25 --> 2014-07-01T13:11:58

A spray surge (identified by AIA and visible at 1330 Å and 1400 Å) occurs during an IRIS limb observation. The IRIS observation shows a jet of material originating at the image's lower right and extending beyond the image's lower left. The spray surge crosses the slit and intensifies common lines (e.g. Mg II h/k). Meanwhile, large coronal rain swaths occupy the observation.

Detected by Jakub Prchlik, Submitted at 2016-08-09T18:54:51

2014-07-03T16:09:47 --> 2014-07-03T19:52:25

Previous AR 12104 observations showed a light bridge splitting a sunspot in half, however, the light bridge nows forms a hard boundary. Evidence for the hard boundary comes from 2796 Å, where the bridge now splits the sunspot oscillations.

Detected by Jakub Prchlik, Submitted at 2016-08-09T18:29:36

2014-07-03T08:00:48 --> 2014-07-03T11:01:25

AR 12104 contains a double-strand light bridge across a sunspot. All observed wavelengths show a light bridge, however, only 1330 Å and 1400 Å show the double strand feature and the bridge's dynamic evolution. While the bottom right strand remains steady, the top left strand spirals through most of the observation. Furthermore, the top left strand does not cross the sunspot until the observation's end.

Detected by Jakub Prchlik, Submitted at 2016-08-09T17:59:53

2014-07-06T07:59:59 --> 2014-07-06T11:00:36

A sunspot in AR 12106 contains oscillations (only visible in 2796 Å). The oscillations are unaffected by a bright filamentary structure that grows and retracts in the sunspot.

Detected by Jakub Prchlik, Submitted at 2016-08-09T14:53:29

2014-07-02T07:59:48 --> 2014-07-02T11:00:25

A coronal hole/sunspot contains two light bridges in AR 12107 (visible in 1330, 1400, 2796, and 2832 Å). The light bridges remain stable for the full exposure (~3 hours). However, the bridges are not static. The bridges display vertically pulsating structures in both 1330 Å and 1400 Å. The sunspot is not static either as it shows oscillations in 2796 Å.

Detected by Jakub Prchlik, Submitted at 2016-08-09T13:52:13

2014-03-15T00:16:56 --> 2014-03-15T00:41:43

AR 12002 produces a GOES C3.1 classified flare (visible in 1330 Å and 1400 Å). The flare's intensity originates from two ribbons, which quickly become (~1-2 frames) two light lobes. After the classified flare subsides, the area shows several brightenings and an unclassified low intensity flare at 03:00. While both events cross the slit, the main flare's spectrum shows a drastic increase in the continuum intensity and in the number of emission lines (e.g., Fe XXI).

Detected by Jakub Prchlik, Submitted at 2016-08-09T13:12:44

2014-03-14T15:39:57 --> 2014-03-14T16:38:23

The coronal rain's intensity and extent fades during an hour long observation in AR 11996.

Detected by Jakub Prchlik, Submitted at 2016-08-09T12:47:52

2014-03-13T23:48:22 --> 2014-03-14T01:22:39

A diffuse cloud in the corona (visible only in 1400 Å) creates streams of coronal rain (visible in both 1400 Å and 2796 Å). Once a coronal rain stream above the cloud interacts with the cloud, the cloud becomes an arch shaped coronal rain structure (00:55:09, visible at 1400 Å and 2796 Å). Even though the cloud structure crosses the slit, the spectrum displays no detectable emission lines from the cloud.

Detected by Jakub Prchlik, Submitted at 2016-08-08T17:47:25

2014-03-16T00:26:48 --> 2014-03-16T01:27:22

The circular triangle sunspot geometry clearly affects the sunspot oscillation's propagation. However, the oscillation's origin is unclear in the image. Therefore, it remains unclear whether each lob in the circular triangle creates its own oscillation or the geometry deflects waves from a central oscillation. 2796 Å clearly shows sunspot oscillations, which are barely visible in 1400 Å. However, 1400 Å shows material emanating near the sunspot's center.

Detected by Jakub Prchlik, Submitted at 2016-08-08T17:47:24

2014-03-14T03:05:02 --> 2014-03-14T03:23:09

Coronal rain over AR 11996 precedes a GOES C4.1 class flare. Both 1330 Å and 1400 Å display the coronal rain and flare. The coronal rain's evolution is similar in both images. Initially, the coronal rain decreases in intensity, however, the coronal rain intensifies approximately a half hour before the flare triggers. The coronal rain intensification increases the coronal rain's footprint on the image and the number of arches (~1 to ~5).

Detected by Jakub Prchlik, Submitted at 2016-08-05T17:58:30

2014-08-04T21:53:04 --> 2014-08-04T22:26:55

IRIS observes a GOES C1.0 flare in AR 12132 (visible in 1330 Å and 2796 Å). The flare forms an sigmoidal pattern between two filaments and crosses the slit. The spectrum shows redshifted emission in common lines (e.g. C II, Si IV, and Mg II h/k).

Detected by Jakub Prchlik, Submitted at 2016-08-05T17:38:52

2014-08-03T06:11:36 --> 2014-08-03T06:40:26

IRIS observes a GOES C1.1 class flare in AR 12132 (visible in 1330 Å and 2796 Å). The flare forms three ribbons, which are connected via an absorption features in 2796 Å and emission in 1330 Å. The ribbons follow the contour of nearby coronal holes and filaments. During the flare, the slit crosses the event showing a spectrum with redshifted emission features (e.g., C II, Si IV, and Mg II h/k).

Detected by Jakub Prchlik, Submitted at 2016-08-05T17:19:46

2014-08-01T06:47:27 --> 2014-08-01T06:54:00

IRIS observes a low intensity flare (no GOES classification). The flare originates on a warm intrusion inside a coronal hole in the image's center. Perhaps due to the flares the location, two horseshoe shaped bright regions create the flare. The flare's spectrum shows a brightening and broadening of common lines (e.g., Si IV and C II).

Detected by Jakub Prchlik, Submitted at 2016-08-05T16:24:47

2014-07-30T02:41:20 --> 2014-07-30T02:52:50

AR 12121 produces a low intensity flare along a coronal filament (primarily visible in 1330 Å). The flare forms two ribbons, one at the base of the filament (center of the image) and another on the side of the filament (top of the image). The flare on the side of the filament creates coronal rain, which extends off the image's edge.