2023 Yoshinori Ohsumi Award for Fundamental Research Awarded to Three Researchers including Associate Professor Mai Sawada

Fluids such as water or gas exist not only on the surface of the earth but also in its interior. Fluids in the earth's crust (crustal fluids) affect seismic activity. Therefore, understanding the spatiotemporal change in crustal fluids with a high resolution of several kilometers and several hours is important. However, it is difficult with conventional methods. In this study, we focus on the changes in the waveform shape of "later phases," which are generated when seismic waves are reflected or scattered by the crustal fluid. Later phases are particularly sensitive to their origin therefore they are useful for detection of the spatiotemporal change in crustal fluids. Our target in this study is later phases observed around the Moriyoshi volcano in Akita, northeastern Japan. Temporal changes in the later phase shapes with several patterns have been reported in this area. The movement of crustal fluid at the later phase origin was pointed out as the main factor of the change in the later phase shape. To reveal the spatiotemporal change in the crustal fluid as the later phase origin in this area, in this study, we classify the waveform patterns of later phases and calculate the waveforms corresponding to each later phase pattern using seismic wave propagation simulations.

Among the stars that light up the night sky, there are 'very massive stars' with more than 100 times the mass of the sun. The intense ultraviolet radiation emitted by these very massive stars has long been thought to blow away the surrounding gas, making it a mystery how they could acquire such a vast mass. However, recent studies have shown that 'disk accretion' is a key factor in this process. In this process, a high-density gas disk diverts ultraviolet radiation in the upward and downward directions of the disk, while simultaneously supplying a large amount of gas to the central star. In our research, we use advanced numerical simulations that consider physical processes such as magnetic fields, radiation, and dust particles to analyze the dynamics of disk accretion and ultraviolet feedback. Furthermore, by collaborating with an international observation project using the ALMA telescope, we aim to validate the birth of very massive stars through disk accretion.