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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0369

Solar jet studies with Hinode, IRIS and Parker Solar Probe

plan term


@ @


 name : Mulay, Bucik, ISSI team (Origins of 3He-Rich Solar Energetic Particles) @  e-mail : sargam[at]iucaa.in, bucik[at]mps.mpg.de

contact person in HINODE team

 name : Culhane, Harra @  e-mail : j.culhane[at]ucl.ac.uk, l.harra[at]ucl.ac.uk

 abstract of observational proposal
Main Objective: To study the relationship of solar jets with solar wind using Parker Solar Probe

Scientific Justification:
The coronal observations of energetic events such as solar jets have given us a new perspective to look at the coronal heating problem and particle acceleration. Jets are short-lived collimated transients and have been observed to originate in different magnetic environments such as coronal holes and activeregions. A multiwavelength study has shown their structure and morphology in different layers of the solar atmosphere (Mulay et al. 2016, 2017). Their association with microflares (Chae et al., 1999), solar X-ray flares
(Mulay et al. 2018), coronal mass ejections (Liu et al., 2015) and solar energetic particle events (Nitta et al., 2006, Bucik et al. 2018a,b) make them interesting for further investigation.

By taking advantage of recently launched Parker Solar Probe satellite which will be at unprecedented
close distance to the Sun, we are interested in studying the properties of the fast (slow) solar wind and
their connection with coronal hole (CH) jets (active region (AR) jets). Furthermore, Parker Solar Probe
would be essential in measuring small-size 3He-rich events.

Depending on the target available on the solar disk during the perihelion, we would like to observe the CH jet or AR jet by using simultaneous imaging and spectroscopic observations from EIS, XRT and IRIS. Our aim is to study the signatures of jets in the transition region and lower corona. We would like to measure the changes in temperature and physical parameters (electron number density, emission measure, plane-of-sky, Doppler and nonthermal velocity etc.) before, during and after the evolution of jet.

It has been observed that most of AR jets originate from the western periphery of active regions and/or leading sunspots (Shimojo et al. 1996). It has been thought that active region edges are the possible sources of slow solar wind. Having signatures of AR jets close to AR outflow regions will advance our understanding of the source region of the slow solar wind. In addition, we would like to study the relationship of jets with 3He-rich particle events and nonthermal type III radio bursts.

Bucik, R., Innes, D.E., Mason, G.M., et al. 2018a, ApJ, 852, 76
Bucik, R., Wiedenbeck, M.E., Mason, G.M., et al. 2018b, ApJL, 869, L21
Chae, J., Qiu, J., Wang, H., Goode, P.R.: 1999, ApJ. Lett. 513, L75
Liu, J., Wang, Y., Shen, C., Liu, K., Pan, Z., Wang, S.: 2015, ApJ, 813, 115.
Mulay, S. M., Tripathi, D., Del Zanna, G., & Mason, H. 2016, A&A, 589, A79
Mulay, S. M., Zanna, G. D., & Mason, H. 2017, A&A, 598, A11
Mulay, S. M., Matthews, S., Hasegawa, T., et al. 2018, Sol. Phys., 293, 160
Nitta, N.V., Reames, D.V., et al. 2006, ApJ, 650, 438
Shimojo, M., Hashimoto, S., Shibata, K., et al. 1996, PASJ, 48, 123

 request to SOT
We would like to have SOT SP observations same as given in HOP 0332 if telemetry permits. If it exceeds the telemetry then we would like to have EIS and XRT observations along with IRIS.

 request to XRT
For on-disk/polar coronal hole and on-disk/limb active region, run the following XRT study.
Filters: Al-poly, Be-thin
Field of view: 512h X 512h
Cadence: 30 sec (or even higher cadence depending the telemetry)

 request to EIS
For on-disk/polar coronal hole: Run the following EIS study.
For on-disk/limb active region: Run the EIS study given for HOP 0332.

EIS study details:
Raster ID: 136
Line list ID: 68
Author: Giulio Del Zanna
Acronym: CAM_QS_2AS_VELO
Title: [RA:000136] [Scan: 9(2h) steps] [ss:2h] [wH:200, nWins:24, LL:000068] [ExpT(Delay) :15.00(0)]
Step Size: 2h
Exposure time : 15.00 sec
Slit: 2h
Window height: 200 pixels
Raster type : Scanning
No. of lines: 24

 other participating instruments
IRIS requests:
For on-disk/polar coronal hole and on-disk/limb active region, run the following IRIS study.

IRIS spectrograph:
OBS ID : 3620109459 | Large sparse 64-step raster 63~120 64s Si IV Mg II h/k Deep ~ 8 Spa | 588.93 |253.62 | 0.3 | 9.2}0.1 | 589}0 | 0.0}0.0 | 18.4}0.0 | 18.4}0.0 | 0.0}0.0

IRIS Slit-Jaw Imager:
Field of view: 120h X 120h
SJI window: Si IV and Mg II
Exposure time: 4 sec
SJI cadence: 18.4 sec

Parker Solar Probe

Dates: ToO - 27 and 28 March 2019, 31 March - 8 April 2019 - during the PSP perihelion.

Time window: We would like the observations to be run for at least 2 hours on 27 and 28 March 2019 prior to the perihelion. During the perihelion, the observation should be run continuously for at least 2 hours from 31 March to 8 April 2019. If time window is April 2-8, 2019 then EIS and IRIS should start to point somewhere on Eastern solar hemisphere (maybe E60) and stop near central meridian (E00).

Target(s) of interest: The above study (for EIS and IRIS) should be run on on-disk/polar coronal hole region covering the part of coronal hole and west boundary of the coronal hole.

The study (HOP 0332 for EIS and above IRIS study) should be run on suitable on-disk active region, pointing at the western side of the leading sunspot region where jets are most likely to be observed.

Previous HOPs:
Dr. Sargam Mulay along with Dr. Helen Mason and Dr. Giulio Del Zanna submitted a proposal HOP 0332 to observe active region jets. We successfully got the observations in 2017. We will be submitting a research paper in a couple of weeks based on this study.

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