7月3日（火）13：30～14：30 理論コロキウム 講義室
Jul 3 Tue DTA colloquium Lecture room
7月3日（火）13：30～15：00 太陽系小天体セミナー 南棟２階会議室
Jul 3 Tue Solar System Minor Body Seminar Conference Room, South Bldg.2F
7月4日（水）10:30～12:00 総研大コロキウム 講義室
Jul 4 Wed SOKENDAI colloquium Lecture Room
7月5日 （木）10:00～11:30 太陽天体プラズマセミナー 院生セミナー室
Jul 5 Thu Solar and Space Plasma Seminar Student Seminar Room, Subaru Bldg.
7月6日（金）16：00～17：00 国立天文台談話会 大セミナー室
Jul 6 Fri NAOJ Seminar Large Seminar Room
詳細は以下をご覧下さい。
7月3日（火）
- Campus
- Mitaka
- Seminar
- DTA colloquium
- Regularly Scheduled/Sporadic
- Regularly Scheduled
- Date and time
- July 3, 2018, 13:30-14:30
- Place
- Lecture room
- Speaker
- Shota Notsu
- Affiliation
- Kyoto University
- Title
- Possibility to locate the position of the H2O snowline in protoplanetary disks through spectroscopic observations
- Abstract
- Observationally locating the position of the H2O snowline in protoplanetary disks is important for understanding the planetesimal and planet formation processes, and the origin of water on Earth. The velocity profiles of emission lines from disks are usually affected by Doppler shift due to Keplerian rotation. Therefore, the line profiles are sensitive to the radial distribution of the line-emitting regions.
In our studies (Notsu et al. 2016, ApJ, 827, 113; 2017, ApJ, 836, 118; 2018, ApJ, 855, 62), we calculated the chemical composition of the disks around a T Tauri star and a Herbig Ae star using chemical kinetics, and then the H2(16)O and H2(18)O line profiles. We found that lines with small Einstein A coefficients and relatively high upper state energies are dominated by emission from the hot midplane region inside the H2O snowline, and therefore through analyzing their profiles the position of the H2O snowline can be located. In addition, we found that H2(18)O lines trace deeper into the disk than H2(16)O lines since the number density of H2(18)O is low (Notsu et al. 2018).
Thus these H2(18)O lines are potentially better probes of the position of the H2O snowline at the disk midplane, depending on the dust optical depth. Moreover, H2(18)O and para-H2(16)O lines with relatively lower upper state energies (~a few 100K) can also locate the position of the H2O snowline. There are several candidate water lines that trace the position of the H2O snowline in ALMA Bands 5－10.
Finally, we have proposed the water line observations for a Herbig Ae disk HD163296 in ALMA Cycle 3, and partial data were delivered. We constrain the line emitting region (the location of the H2O snowline) and the dust properties from the observations. - Facilitator
- -Name：Tomoya Takiwaki
- Comment
- in English
7月3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
- 7月3日（火曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 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
7月4日（水）
- Campus
- Mitaka
- Seminar
- SOKENDAI colloquium
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- July 4, 2018, 10:30 -12:00
- Place
- Lecture Room
- Speaker
- Takafumi Tsukui
- Affiliation
- SOKENDAI 2nd year (M2)(Supervisor: Satoru Iguchi,Hiroshi Nagai,Yuichi Matsuda)
- Title
- Exploring Dark Matter Profile of the Galaxy NGC1380 with ALMA
- Abstract
- Please note that the presenter information posted here is not necessarily listed in order of presentation.
- Facilitator
- -Name：Yoshiki Hatta
- Comment
- TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.
7月5日（木）
- Campus
- Mitaka
- Seminar
- Solar and Space Plasma Seminar
- Regularly Scheduled/Sporadic
- Sporadic
- Date and time
- 5 July (Thu), 10:00-11:30
- Place
- Student Seminar Room, Subaru Bldg.
- Speaker
- Yu Liu
- Affiliation
- Yunnan Observatories
- Title
- Operation of the monitoring stations at Mt.Wumingshan and proposals of our future coronagraphs
- Abstract
- The Wumingshan mountain (Mt. WMS), located in the Grand Shangri-La area of south-west China, has been selected as one of the most potential regions for hosting China’s next-generation ground-based large telescopes, since Mt. WMS owns ideal astronomical conditions for both day-time and night-time observations. In October 2014, we initiated a long-term monitoring task in Mt. WMS. We have been collecting data from two monitoring sites for more than three years. Both sites are located about 4700-4800 m above the sea level. Our instruments mainly include the solar and stellar Differential Image Motion Monitors, the Sky Brightness Monitors, the PWVC monitors, the Atmospheric Temperature Fluctuation Monitors, the Multi-wavelength Solar Photometers and robot meterological stations, and so on. In this talk, we present the daily observation, transmission, storage and analysis of the harvested data, and the overall operation, management and technical support of the monitoring platforms. A few solar coronagraph projects are also briefly introduced.
- Facilitator
- -Name：Shin Toriumi
- Comment
7月6日（金）
- Campus
- Mitaka
- Seminar
- NAOJ seminar
- Regularly Scheduled/Sporadic
- Scheduled
- Date and time
- Fri 6 July. 16:00~17:00
- Place
- Large Seminar Room
- Speaker
- Chris Packham
- Affiliation
- University of Texas
- Title
- ” An Update on MICHI for the TMT and Some International Perspectives ”
- Abstract
- The field of thermal-IR astronomy will soon enjoy a revolution when the JWST is launched. It is easy to imagine that all areas of IR astronomy will be greatly advanced, but perhaps impossible to conceive of the new vistas that will be opened. Many of these discoveries will require follow-up observations at higher spectral and spatial resolution than JWST can provide. Therefore, we are now designing science cases and an instrument for MICHI (Mid-IR Camera, High-disperser & IFU spectrograph), a thermal-IR imager and spectrometer for early operation on the Thirty Meter Telescope (TMT). I provide updates to the driving science cases for MICHI. The science and instrumentation teams include representatives from all countries of the TMT consortium, and I comment on the advantages and challenges of the international nature of such instrument teams.
- Facilitator
- -Name： Matsuda, Yuichi