6月 6日（火）13：30～ ： 太陽系科学セミナー 講義室
Jun 6 tue Solar System Science Seminar Rinkoh Seminar Room
6月 7日（水）10：30～12：00 総研大コロキウム 中央棟 講義室
Jun 7 wed SOKENDAI colloquium Lecture Room
6月 7日（水）13：30～14：30 理論コロキウム コスモス会館会議室
Jun 7 wed DTA colloquium Conference Room, Cosmos Lodge
詳細は以下をご覧下さい。
6月6日（火）
- キャンパス
- 三鷹
- セミナー名
- 太陽系科学セミナー
- 定例・臨時の別
- 定例
- 日時
- 6月6日（火曜日）13時30分～
- 場所
- 講義室
- 講演者
- 伊藤孝士
- タイトル
- 【活動的小惑星勉強会 2】(3200)Phaethonに関する知見の一部の紹介
- Abstract
- 投稿中の論文arXiv:1703.00296で発表された分光・測光観測結果に主
に沿い、これまで多種多様な研究が為されて来た近地球小天体(3200)Phaethonに
ついて先行研究の結果も含めた現時点での知見の極く一部の概観の要約を試み
る。今回は当該勉強会の性質を鑑み、多くの箇所で視聴者参加型の形式を採る。
なお本講演の多くの部分は平成29年5月16日開催の第19回CPS月惑星探査研究会
(DESTINY+ミニワークショップ)での発表に重なる事を予めお断りする。
https://www.wakusei.jp/~postmaster/ml/postmaster-oml/2016/msg00753.html - 世話人
-
-名前：脇田茂
-名前：松本晃治
-名前：土屋智恵
6月7日（水）
- Campus
- Mitaka
- Seminar
- SOKENDAI colloquium
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- June 7 2017, 10:30-12:00
- Place
- Lecture Room
- Speaker1
- Nagaaki Kambara
- Affiliation
- SOKENDAI D1 (Supervisor; T. Sekii; T. Watanabe; M. Kubo) Title:Solar convective velocity measurements by ring diagram method
- Speaker2
- Yoshiki Hatta
- Affiliation
- SOKENDAI M2 (Supervisor; T. Sekii)
- Title
- structure inversion in helioseismology
- Facilitator
- -Name：Misaki Ando
- Comment
- TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.
6月7日（水）
- Campus
- Mitaka
- Seminar
- DTA colloquium
Regularly Scheduled - Date and time
- June 7th, 2017, 13:30-14:30
- Place
- Conference Room, Cosmos Lodge
- Speaker
- Tomoya Kinugawa
- Affiliation
- University of Tokyo
- Title
- Compact binary remnants from first stars for the gravitational wave source
- Abstract
- (optional)
Using our population synthesis code, we found that the typical chirp mass of binary black holes (BH-BHs) whose origin is the first star (Pop III) is ~30 Msun. This result predicted the gravitational wave events like GW150914 and LIGO paper said “recently predicted BBH total masses agree astonishingly well with GW150914 and can have sufficiently long merger times to occur in the nearby universe (Kinugawa et al. 2014)” (Abbot et al. ApJL 818,22 (2016)). Thus, the compact binary remnants of the first stars are interesting targets of LIGO,VIRGO and KAGRA.Nakano, Tanaka & Nakamura 2015 show that if S/N of QNM is larger than 35, we can confirm or refute the General Relativity more than 5 sigma level. In our standard model, the detection rate of Pop III BH-BHs whose S/N is larger than 35 is 3.2 events/yr (SFR_p/(10^{-2.5}Msun/yr/Mpc^3))*([f_b/(1+f_b)]/0.33)* Err_sys. Thus, there is a good chance to check whether GR is correct or not in the strong gravity region. Furthermore, the Pop III binaries become not only BH-BH but also NS-BH. We found Pop III NS-BH merger rate is ~ 1 events/Gpc^3 and the chirp mass of Pop III NS-BH is more massive than that of Pop I and II. Therefore, we might get information of Pop III stars from massive BH-BHs and NS-BHs. - Facilitator
- -Name：Tomoya Takiwaki
- Comment
- in English
以上