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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0354

Probing the chromosphere of coronal holes and coronal hole boundaries. Support for ALMA observations

plan term


@ @


 name : Loukitcheva, Solanki, White, Leenaarts, Carlsson, Gary @  e-mail : lukicheva[at]mps.mpg.de

contact person in HINODE team

 name : Savage, Watanabe, De Pontieu
@  e-mail : sabrina.savage[at]nasa.gov, watanabe[at]uvlab.mtk.nao.ac.jp, bdp[at]lmsal.com

 abstract of observational proposal
Main Objective:
We aim to study the dependence of chromospheric structure and heating on the magnetic field's topology and to search for signs of enhanced heating produced by magnetic reconnection at coronal hole boundaries.

Scientific Justification:
With dual-band ALMA observations coordinated with Hinode-IRIS observations we aim to answer the specific questions on how the chromospheric structure in coronal holes, as inferred from the observed images, differ from that in the normal quiet Sun, whether the difference in the magnetic field topology influences the heating of the chromospheric gas, as inferred from the temperatures measured by ALMA in the two regions, and what are the chromospheric signatures of the magnetic reconnection at the boundaries between QS and CH, as inferred from transient activity seen by comparing multiple images for the same region.

 request to SOT
SP fast maps 164"x164" full FOV, 0.32" sampling, ~30 minute/map.

 request to XRT
Standard request from ALMA support HOP 328, Al-mesh & thin-Be, better than 3 mins cadence, FoV: 128"x128"(384"x384", if telemetry available).

Filters could be adjusted to accommodate current instrument and solar conditions.

 request to EIS

 other participating instruments
ALMA: #1141
After discussion with Bart De Pontieu, priority is to obtain the high data rate versions. If telemetry is low and/or memory is close to full during this day, please pause observations before or after the ALMA observations and only use low data rate alternative if absolutely necessary.

Please roll to an angle as close as possible to the ALMA request (if there are roll angle restrictions, please try to get to the closest angle to the ALMA requested angle).

For band 3 observations:
3620604059 | Large sparse 64-step raster 63x120 64s Deep x 2 Spatial x 2, Spectra | 199.20 | 189.48 | 0.7 | 3.1+/-0.1 | 199+/-0 | 12.5+/-0.0 | 12.5+/-0.0 | 12.5+/-0.0 | 12.5+/-0.0

low data rate alternative
3640604059 | Large sparse 64-step raster 63x120 64s Deep x 2 Spatial x 2, Spectra | 196.10 | 124.60 | 0.4 | 3.1+/-0.1 | 196+/-0 | 12.3+/-0.0 | 12.3+/-0.0 | 12.3+/-0.0 | 12.3+/-0.0

For band 6 observations:
3620604072 | Large dense 192-step raster 63.1x120 192s Deep x 2 Spatial x 2, Spec | 597.60 |

568.44 | 0.7 | 3.1+/-0.1 | 598+/-0 | 12.5+/-0.0 | 12.5+/-0.0 | 12.5+/-0.0 | 12.5+/-0.0

low data rate alternative:
3640604072 | Large dense 192-step raster 63.1x120 192s Deep x 2 Spatial x 2, Spec | 588.29 | 373.80 | 0.4 | 3.1+/-0.1 | 588+/-0 | 12.3+/-0.0 | 12.3+/-0.0 | 12.3+/-0.0 | 12.3+/-0.0 .

Dates: The ALMA observations will take place in April 2018

Time window: To be observed for 4 hours total (2 hours in each ALMA band) during ALMA day time, 13 -20 UT.

Target(s) of interest: An on-disk mid-latitude coronal hole to include also a part of QS, covering an area of dimension 120" x 60" in ALMA FoV, with the longer axis lying orthogonal to the coronal hole boundary to provide roughly equal areas of QS and CH. The pointing will be decided given the ALMA constraints.

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