Coronal hole plume observation, 19 & 21-Mar-2016

There was a medium size coronal hole passing the central meridian on 19-Mar-2016 so I requested a run of IHOP 266. I was also given another observation on 21-Mar-2016. Thanks go to the IRIS planner, Danny Ryan, and the EIS planner, Kyoung-Sun Lee, for getting this observation run.


I chose a bright plume close to the south boundary of the coronal hole. The plume was very bright and was quite dynamic during the observation. The movie below shows AIA 171 at 5min cadence, with the position of the EIS slit overplotted as a narrow rectangle. The EIS pointing was derived using the method described on the EIS wiki, applying the EIS-AIA offset, and so it should be fairly accurate.

AIA 171 movie at 5 minute cadence. Logarithmic intensity scaling.

The EIS files have the following times:

12:04  PRY_slot_context_v3
12:07  Cool_loop_stare
13:05  Cool_loop_stare
14:02  Cool_loop_stare
14:59  Cool_loop_stare
15:56  Cool_loop_stare
16:53  PRY_slot_context_v3

The IRIS files have the following times:

12:14-14:35  32 rasters (16-step)
14:57-16:12  17 rasters
16:39-17:32  12 rasters

The XRT observation from the CO's notes was:

XOB #1B1E: CH Al/poly+Thin-Be-256x256-1min cad-AEC0-HOP266, with G-band
(3ms/3ms VLS=CLS)
03/19 12:03:00 - 03/19 18:00:00 : IHOP 266: Coronal hole plume obs.

The SOT CO chose not to support HOP 266.


The IRIS observation as printed in the planner's notes was:

+2 12:09-16:56     HOP 266: Small-scale reconnection in coronal hole plumes [408", 350"]

EIS used a raster study this time:

12:03-12:06   PRY_slot_context_v3
12:06-15:46 Cool_loop_resp_v2 [14 repeats]
15:46-15:49 PRY_slot_context_v3

Note that both EIS and IRIS ran CH boundary studies after this observation.

The movie below shows the location of EIS slit during the sequence. The target is the same as 19-Mar, but it has evolved since then.

AIA 171 & 193 movie at 5 minute cadence with EIS slit. Logarithmic intensity scaling.

Page maintained by Dr Peter Young.