Welcome to my website! I am Takahiro Ueda, a JSPS Research Fellow (PD) working at National Astronomical Observatory of Japan. I have been working on the dust evolution in protoplanetary disks with a particular interest in how terrestrial planets form. I got my Ph.D. at Tokyo Institute of Technology on March 2019 under the supervision of Prof. Shigeru Ida with co-supervised by Prof. Satoshi Okuzumi. After that, I moved to NAOJ as a JSPS Fellow and am studying the inner region of disks by using numerical simulations and observations with such as ALMA with Prof. Akimasa Kataoka.
Name: Takahiro UEDA (植田 高啓)
Current Status: JSPS Research Fellow (PD)
Affiliation: National Astronomical Observatory of Japan
Email: takahiro.ueda_at_nao.ac.jp / takahiro.ueda.astro_at_gmail.com
The institute email address sometimes lose emails recently. In case you could not get a response, please use the gmail one.
Address: Central Building (South) 318, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, JAPAN
There are longstanding questions about planets:
How do they form?
Are there other planets similar to our Earth?
When and how did life rise on our Earth?
With the goals to answer these questions, I'm working on the planet formation through astrophysical numerical simulations and observations.
Formation of Planets
Dust growth is a first step of planet formation. In protoplanetary disks, the birthplace of planets, micron-sized dust particles collide each other, coagulate into larger bodies and eventually grow into planets. I'm trying to reveal where and how do planets are formed from small grains particularly using dust-growth simulations and radiative transfer simulations.
Dust Growth in Protoplanetary Disks
In our solar system, there are many dust grains originating from asteroid collisions and cometary activities. These grains are visible in a clear sky and some of them fall onto our Earth. These grains provide us keys to understand the formation process of fragments and their parent body. I'm investigating the properties of the dust particles using orbital calculations.