Hinode Seminar 2019 (Log)


Place: Hiinode meeting room (#1754) at Building A, 7-F
Regular Time: 16:00-17:30 on Monday
Organizer: Tomoko Kawate


Upcoming seminar schedule

Dr. Iwai (Nagoya Univ.) - May 20
Dr. Sterling (NASA) - May 23
Mr. Hasegawa (ISAS) - mid June


May 23 (Thu) Dr. A. C. Sterling (NASA)
Update on Coronal Jets, and Their Connections to Other Solar Features
We review recent ideas about solar coronal jets and their causes. Many --- if not most or all --- such jets result from the eruption of small-scale filaments, or "minifilaments." Moreover, more recent work has confirmed earlier hints that magnetic flux cancelation is often the trigger that induces eruption of the minifilaments. While typical coronal jets have base size sizes of ~10,000 km. We present evidence for smaller-scale jet features, called "jetlets, which have base sizes ~4000, are seen in EUV and UV, and which occur in the network; we consider whether jets extend down to the size of chromospheric spicules (widths ~300 km). We then consider the opposite size scale, of the size of small active regions, and show how coronal jets are starting to provide clues to the mechanism that drives larger-scale CME-producing eruptions.

May 20 (Mon) Dr. K. Iwai (Nagoya Univ.)
Heliospheric Physics and Space Weather with Interplanetary Scintillation Observations
Interplanetary scintillation (IPS) is a radio scattering phenomenon caused by the disturbances in the solar wind. The ground-based IPS observation has been an important technique to investigate the heliosphere. Now, we are going to have many opportunities to investigate the solar corona and its connection to the inner heliosphere such as PSP, MMO, Solar orbiter, and Solar-C_EUVST. The synergy between these instruments and ground-based IPS observations should be a key issue for us. We have developed an IPS estimation system based on a global magnetohydrodynamic (MHD) simulation of the inner heliosphere. In this system, the background solar wind and propagation of the CMEs are calculated by a global MHD simulation. The IPS response is estimated by the three-dimensional density distribution of the inner heliosphere derived from the MHD simulation. The simulated IPS response is compared with the actual IPS observations made by ISEE, Nagoya University, to achieve more realistic simulation result. Now, this system has been installed in the space weather forecasting system in NICT to predict the arrival time of CMEs. This system is also useful to compare the IPS data with other space-based observational data.

May 8 (Wed) Mr. Y. Kawabata (ISAS)
Observational Studies on Non-potential Magnetic Field in Solar Active Regions
Solar active regions sometimes produce explosive events, such as solar flares and coronal mass ejections causing several influences to the geomagnetic environment. The main interest of our study is how the non-potential magnetic field is distributed in active regions. The measurements of the magnetic field have been mainly performed at the photospheric height. The coronal magnetic field through polarimetric observations are difficult even with the state-of-art instruments. To overcome the difficulty, the nonlinear force-free field (NLFFF) modeling has been extensively used to infer the three-dimensional (3D) magnetic field in the solar corona. We attempt to investigate the non-potential magnetic field and its 3D structure in active regions, while we tackle the technical problem in the NLFFF modeling. We focus on two different viewpoints with the NLFFF modeling and observations. (1) We investigate the robustness and dependency of the NLFFF calculation with respect to the initial guess of the 3D magnetic field. While previous studies often use potential field as the initial guess in the NLFFF modeling, we adopt the linear force-free fields with different constant force-free alpha as the initial guesses. (2) We examine the direct measurements of the chromospheric magnetic field in the whole active regions through the spectropolarimetric observations at He I10830 A. The results of NLFFF extrapolation from the photosphere are compared with the direct measurements. We obtained following findings. (1) The dependency of the initial condition in the NLFFF extrapolation is smaller in the strong magnetic field region. Therefore, the magnetic field at the lower height tends to be less affected by the initial condition. (2) Chromospheric magnetic field may have larger non-potentiality compared to the photospheric magnetic field. The large non-potentiality in the chromospheric height may not be reproduced by the NLFFF extrapolation from the photospheric magnetic field. The magnitude of the underestimation of the non-potentiality at the chromospheric height may reach 30-40 degree in signed shear angle. We conclude that the magnetic field in the upper atmosphere may have higher non-potentiality than previously thought based on the NLFFF. Because the non-potentialty is crucial in the MHD instability, this finding will improve understand onset mechanism for solar flares and CMEs, which affect the environment in the solar system.

Apr 22 (Mon) Dr. T. Shimizu (ISAS) PDF
Recent progress and future prospects in solar observations
With a brief summary of recent progress in solar observations, I will discuss future prospects of solar researches for 2020s and beyond. The discussion will cover new projects and what I want to do in 2019 and coming years.