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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0298

Coordinated Hinode/EIS and ground based observations of the total solar eclipse of 9 Mar 2016

plan term


@ @


 name : Landi, Habbal @  e-mail : elandi[at]umich.edu, shadia[at]ifa.hawaii.edu

contact person in HINODE team

 name : Landi @  e-mail : elandi[at]umich.edu

 abstract of observational proposal
The total eclipse taking place on 2016 March 9 (at around 00:40 UT) will be observed from the ground in Indonesia with a suite of filters designed to isolate and measure the intensity of visible lines from Fe XI and Fe XIV and in white light. Also, we will have a dual channel spectrometer centered around the same Fe XI and XIV lines which will provide us with measurements of the full line profile. As the field of view of the observation will extend from the limb up to 4 solar radii, these measurements will provide a unique window on the physical properties of the extended solar corona, providing us with AIA-like 2D images of the solar corona, which hold the additional advantages over AIA of 1) better spectral/temperature purity, 2) 10 times larger effective field of view, and most importantly 3) the same plasma diagnostic capabilities of EIS.

Emission lines in the visible are formed by radiative scattering of disk emission starting from approximately 1.1 Rsun. The combination of visible spectral lines with 1) collisionally dominated EUV coronal lines from EIS and 2) visible observations of the background continuum will allow us to apply unique spectroscopic diagnostic techniques that will provide:

1 - The first ever empirical determination of fast and slow solar wind freeze-in heights for Fe;

2 - The empirical determination of frozen-in Fe charge state ratios to be directly compared with in-situ data;

3 - An empirical model of the fast and slow wind velocity, electron temperature and electron density profiles from the limb to the freeze-in region using the novel technique developed by Landi et al. 2012 (ApJ, 750, 159)

4 - Large scale distributions of plasma parameters (electron density, temperature and filling factor) in streamers and coronal holes.

COMP observations of the Fe XIII 10747 and 10800 line pair will allow the determination of the electron density below 1.5 solar radii to be compared with Hinode/EIS determinations, as well as cross-calibration between EIS, COMP and the eclipse observations.

We propose supporting observations from Hinode/EIS and Hinode/XRT during the eclipse, and for a few hours before and after the eclipse on 2016 March 9 The targets will be slowly evolving large-scale coronal structures (active region, streamer and coronal holes) before, during and after the eclipse. We would like to have EIS observations at the East limb, to better coordinate with the spectrally resolved observations from the dual spectrometer.

During the eclipse we would like to observe a prominence cavity at the limb, which will allow us to easily co-align EIS observations with eclipse images. In the absence of a cavity, we will observe an active region at the limb.

 request to SOT

 request to XRT
Time series of images at the solar limb

TARGET: same as EIS

FIELD OF VIEW: 512x512 (384x384 acceptable)

EXPOSURE TIME: Long exposure time (AEC setting = 2)

FILTERS: Al/poly, Ti/poly and Al/mesh

CADENCE: It can be slow, we are not looking for sudden events

Simultaneous observations with EIS

 request to EIS
(raster size with JPEG90 compression)

If a cavity is available (PCH=Polar Coronal Hole):

1 - The first ever empirical determination of fast and slow solar wind freeze-in heights for Fe;

2 - The empirical determination of frozen-in Fe charge state ratios to be directly compared with in-situ data;

Program Target Timing Size(Mb) Duration
dhb_polar_scan Streamer/PCH Before eclipse 383.0 3h 46m
gdz_plume1_2_300_50s cavity During eclipse 165.0 1h 8m
Total 548.0 5h 54m

If no cavity is available:

Program Target Timing Size(Mb) Duration
dhb_polar_scan Streamer/AR Bef/dur eclipse 383.0 3h 46m
landi_scan_ch coronal hole After eclipse 190.0 2h 7m
Total 573.0 5h 53m

Simultaneous observations with XRT

 other participating instruments

DURATION: Approximately 5 hours WHEN: Around 2016 March 9, 00:40 UT

POINTING: We would like to have EIS and XRT observing at the East solar limb. The pointing can be easily achieved having SOT pointing on the disk within 15-20 arcsec from the limb, and using the EIS fine mirror mechanism to point at the targets.

During the eclipse: Cavity (if available - PRIMARY target)
Limb active region (if cavity unavailable - BACKUP target)

Before and after the eclipse: polar coronal hole/streamer boundary (if available)
streamer (if polar holes are not available)

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