HOP 0464

proposer

name :

Kawabata, Ishikawa, Okamoto, Oba, Katsukawa, Kubo, Ishikawa, Tei, Asensio Ramos, Quintero Noda, Matsumoto, Iijima

e-mail :

kawabata.yusuke[at]nao.ac.jp, ryoko.ishikawa[at]nao.ac.jp, joten.okamoto[at]nao.ac.jp, takayoshi.oba[at]nao.ac.jp, yukio.katsukawa[at]nao.ac.jp, masahito.kubo[at]nao.ac.jp, ryohtaroh.ishikawa[at]nao.ac.jp, tei.akiko[at]jaxa.jp, andres.asensio[at]iac.es, carlos.quintero[at]iac.es, takuma.matsumoto[at]nagoya-u.jp, h.iijima[at]isee.nagoya-u.ac.jp

abstract of observational proposal

Main Objective:
Quantitatively obtain the magnetic and velocity oscillations in the photosphere and chromosphere, and reveal the phase relationship between them.

Scientific Justification:
Magnetohydrodynamic (MHD) waves are thought to play an important role in heating the plasmas in the solar atmosphere. The stable high resolution imaging observations with Hinode spacecraft showed the evidence of the MHD waves in the prominences (Okamoto et al. 2007) and spicules (He et al. 2009). In addition to the imaging observations, the spectropolarimetric observations in the photosphere enabled the quantitative analysis of the MHD waves in the sunspots (Fujimura & Tsuneta 2009). The multi-wavelength observations with Vacuum Tower Telescope showed the wave propagation from the photosphere to the chromosphere (Felipe et al. 2010). To evaluate the dissipation, the energy flux and mode of the MHD waves, the magnetic and velocity field measurements are mandatory. As a next step, we would like to diagnose the MHD waves in the chromosphere quantitatively. The observation of MHD waves in the chromosphere is also an important topic from the viewpoint of the elementary process of plasma physics in a weakly ionized environment.

The purposes of our observations are to quantitatively obtain the magnetic and velocity oscillations from the photosphere to the chromosphere and to reveal the phase relationship between them by spectropolarimetric observations with Hinode, IRIS, and GREGOR

other participating instruments

IRIS requests: We request at least for 2 hrs (8:00-10:00 UT,) with required cadence. After 10:00 UT, the cadence might be reduced depending on telemetry.
Candidate program:
3600100038 | Medium sparse 16-step raster 15x60 16s Spatial x 2, Spectral x 2 | 34.08 |34.19 | 0.68 | 2.1+/-0.1 | 34.1+/-0.0 | 17.0+/-0.0 | 17.0+/-0.0 | 17.0+/-0.0 | 17.0+/-0.0
Raster FOV 15’’x 60’’ or 15”x120” (ID 3600100039 if telemetry allows),
raster mode sparse raster 1’’,
raster cadence 20-30 sec or around, exposure time 1 sec or 2 sec,
Lines: Large Line List (Mg II h/k and Mg II wing should be included)
slit-jaw 2796/2832/1330/1400
The pointing and OBS ID information will be given by Y. Kawabata

Additional instrument coordination: GREGOR/GRIS

remarks

Dates: 4/11/2023-4/20/2023

Time window: We request the daytime in Tenerife between 8:00 UT-12:00 UT (minimum: 8:00 UT-10:00 UT).

Target(s) of interest: Main target is an active region filament. In case there are no active region filaments during the campaign, we will observe the optional targets, such as plages and/or sunspot umbrae.

Previous HOPs:
HOP346. We requested the coordination observation of Active region with GREGOR and Hinode and the HOP was run once. Unfortunately, active regions did not appear during the campaign. There is no outputs from the HOP.