Research
Theory & Observation of
the Formation of Stars and Planets across Cosmic History
Feedback in Massive Star Formation
In the universe, there are stars that are hundreds of times more massive than our sun. How do such massive stars form under the intense radiative feedback? We investigate the process of massive star formation through theory [Tanaka et al. 2017, etc.] and observation [Zhang, Tanaka, et al. 2019, etc.].
Hot-Disk Chemistry & Dust
Recent high-resolution ALMA observations have shown that massive protostellar disks are extremely hot and dynamical, and some refractory molecules, such as silicon compounds and sodium chloride, are detected as the gaseous form [Tanaka et al. 2020, etc.]. Observations of those "hot disks" provide new insights into the evolution of silicate dust and the origin of meteoritic high-temperature condensations, which are difficult by observations of lower-temperature protoplanetary disks [e.g., Yamamuro, Tanaka, & Okuzumi 2023].
Low-metallicity Star Formation
Throughout cosmic history, the galactic environment has undergone significant changes. How did stars and planets form in the low-metallicity early universe? To bridge the gap between the present-day and early universes, we investigate low-metallicity star formation from theoretical [Tanaka et al. 2018, etc.] and observational [Shimonishi, Tanaka et al. 2023, etc.] perspectives.
Synthetic Observational Modeling
Theoretical models are essential for deciphering 3D structures and kinematics from observation data, while observational tests are necessary to improve theoretical models. As a key tool to connect theory and observation, we are developing synthetic observational models [Tanaka et al. 2016, etc].
