APR 26 Tue 10:00～11:30 太陽系小天体セミナー / Solar System Minor Body Seminar zoom
APR 27 Wed 10:30～12:00 SOKENDAI Colloquium zoom
APR 27 Wed 15:30～17:00 NAOJ Science Colloquium zoom
詳細は以下をご覧下さい
4月26日（火）
キャンパス：三鷹
セミナー名：太陽系小天体セミナー
定例・臨時の別：定例
日時：4月26日（火曜日）10時00分～11時30分
場所：zoom
講演者：渡部潤一
世話人の連絡先
名前：渡部潤一
備考：テレビ会議またはスカイプによる参加も可
4月27日（水）
Campus：Mitaka
Seminar：SOKENDAI Colloquium
Regularly Scheduled/Sporadic：Regular
Date and time：April 27th, 2022 10:30-12:00
Speaker 1：Rikuto Omae
Affiliation：SOKENDAI 4th year (D2) (Supervisor: Mami Machida, Masami Ouchi, Kazuhiro Hada)
Title：Observability of magnetic field in lensing galaxies using broadband radio polarization data
Speaker 2：Shotaro Tada
Affiliation：SOKENDAI 3rd year (D1) (Supervisor: Takayuki Kotani, Yutaka Hayano, Yosuke Minowa)
Title：Detector calibration experiments for very high precision photometry and astrometry from space
Facilitator
-Name：Matsuda, Graduate Student Affairs Unit
4月27日（水）
Campus：Mitaka
Seminar：NAOJ Science Colloquium
Regularly Scheduled/Sporadic：Every Wednesday
Date and time：2022 April 27, 15:30-17:00
Place：zoom / Instrument Development Bldg. 3 (hybrid)
Speaker：Ayaka Okuya
Affiliation：NAOJ
Title：Modeling of accretion disks originating from disrupted planetary bodies around white dwarfs
Abstract：From a quarter to a half of WDs have rock-forming elements in their atmospheres, and some of them show infrared excess from their circumstellar dusty disks. These are thought to be originated from the tidally disrupted minor planets. Therefore, the metals in the WD atmospheres would enable us to directly measure the elemental composition of exoplanetary bodies with unprecedented precision. Moreover, the dynamical arguments based on the delivery rate of minor planets to the Roche limit could provide unique insights into the planetary system architecture orbiting around WDs.
In this study, as a first step to establishing the framework that can derive such information from observations, we develop the first accretion disk model that solves the coupled evolution of multiple materials. We find that the disks produced by the disrupted rocky bodies cannot reproduce the observed high accretion rate due to the rapid re-condensation of diffused-out vapor just outside the silicate sublimation line. In the case of icy body accretion, the volatile vapor can enhance the silicate accretion rate through gas drag to successfully achieve the observed high accretion rate. We find that, however, a high silicate accretion rate is always accompanied by a comparably high volatile accretion rate, resulting in the volatile-rich photospheric composition. This is inconsistent with the observed photospheric composition. No solution that reproduces observations implies that the existing disk models miss some physical processes and/or that the current data interpretation method might have some problems. I will finally discuss the future direction of this study.
Facilitator
-Name：Akimasa Kataoka
Comment：English