(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.
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.
Liu, J., Wang, Y., Shen, C., Liu, K., Pan, Z., Wang, S.: 2015, ApJ, 813, 115.
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.
For on-disk/polar coronal hole and on-disk/limb active region, run the following XRT study.
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.
For on-disk/polar coronal hole and on-disk/limb active region, run the following IRIS study.
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.
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.