7th Asia-Pacific Conference on Plasma Physics, 12-17 Nov, 2023 at Port Messe Nagoya

Observational study of intermittent solar jets with the Goode solar telescope

Guiping Ruan1, Qiuzhuo Cai1, Chenxi Zheng1, Brigitte Schmieder2,3, Jinhan Guo 2,4 , Yao
Chen1,Jiangtao Su5, Yang
1Liu , Jihong Liu6 , and Wenda Cao7,81 Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute ofSpace Sciences,Shandong University, Weihai 264209, ChinaCentre for Mathematical Plasma-Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B,3001 Leuven,Belgium
3LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place JulesJanssen, 92190 Meudon, France
4
School of Astronomy and Space Science and Key Laboratory for Modern Astronomy and Astrophysics, Nanjing
University, Nanjing 210023, China
5 National Astronomical Observatories, Chinese Academy of Sciences
6Shijiazhuang University, Shijiazhuang
7Center for Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Blvd.,Newark, NJ 07102, USA
8Big Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92316, USA2e-mail (speaker): rgp@sdu.edu.cn
We studied intermittent jet events using
motion of the granulation in the photospheredata from instruments on the Goode Solardrives the magnetic reconnection. TheTelescope at the Big Bear Solar Observatoryintermittent jet events we studied are triggered(BBSO) derived from the TiO image of theby magnetic reconnection process which is
wideband Imager (BFI), the Hα image of themodulated by p-mode oscillations.
visible Light Spectrometer (VIS), and theCompared with the quiet region of the sun,magnetic fields of the near-infrared spectral
we found that the root of intermittent jets arepolarizer (NIRIS). In addition, we also usedenhanced at the center of the Hα spectral line
Slit-Jaw Imager (SJI) data from the Interface
profile, but there is no significant change on theRegion Imaging Spectrograph (IRIS). These
two sides of the line wing, which indicates thatobservations allow us to better characterize thethere may be a long time heating phenomenon
burst jets. We found that the right of the mainat the root of intermittent jets.
sunspot continued to erupt plasma material for
References:[1] Roy, J. R. 1973, SoPh, 28, 95
up to 4 hours on August 6, 2016, NOAA AR[2] Shibata, K., Ishido, Y., Acton, L. W., et al. 1992,12571. The time distance diagram shows that
PASJ, 44, L173
the peak of the jet has obvious periodic[3] Hong, Z., Wang, Y., & Ji, H. 2022, ApJ, 928, 153
eruption characteristics (5 minutes) during[4] Jiang, Y. C., Chen, H. D., Li, K. J., Shen, Y. D., &18:00 UT-18:50 UT. We also found periodic
Yang, L. H. 2007, A&A, 469, 331
brightening phenomenon (5 minutes) during[5] Li, H. D., Jiang, Y. C., Yang, J. Y., Bi, Y., &jets bursts in the observed bands in thetransition Region(1400Å and 2796Å), which
may be a response to intermittent jets in theupper solar atmosphere. The time lag is 3minutes. The evolution image of TiO bandshows horizontal movement of granulation atjets position. We suggest that the horizontal

Liang, H. F. 2015, Ap&SS,359, 4[6] Wang, Y., Zhang, Q., & Ji, H. 2021, ApJ, 913, 59[7] Zhao,Jie, Chromospheric Recurrent Jets in a
Sunspot Group and Their Intergranular Origin,2022,ApJ, 932, 95