5月23日（火）13：30～15：00 太陽系小天体セミナー 南棟２階会議室
May 23 tue Solar System Minor Body Seminar Conference Room, South B
5月24日（水）10：30～12：00 総研大コロキウム 大セミナー室
May 24 wed SOKENDAI colloquium Large Seminar Room
5月24日（水）13：30～14：30 理論コロキウム コスモス会館会議室
May 24 wed DTA colloquium Conference Room, Cosmos Lodge
5月26日（金）13：30～15：00 太陽天体プラズマセミナー 院生セミナー室
May 26 fri Solar and Space Plasma Seminar Student Seminar Room, Subaru Bldg.
5月26日（金）16：00～17：00 国立天文台談話会 大セミナー室
May 26 fri NAOJ Seminar Large Seminar Room
詳細は以下をご覧下さい。
5月23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
- 5月23日（火曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 講演者
- Dan Boice
- タイトル
- SUISEI: A Versatile Physicochemical Model for Small Solar System
- Abstract
- A suite of computational tools, named SUISEI, has been developed over the past decades and successfully applied to interpret observations of comets. A brief overview of SUISEI will be given; including ComChem, a global, multifluid gas dynamics simulation with detailed chemical kinetics of the cometary coma; coupled with ComDust, a model of comet dust evolution and interaction with gas; and ComNuc, a 3-D simulation of gas and heat flow within the comet nucleus porous subsurface layers. The combination of these tools have resulted in an improved knowledge of chemical species that form in cometary environments and their relationship to native molecules that exist in the nucleus ices by analyzing space- and ground-based observations and in situ measurements by instrumentation onboard spacecraft missions.
This model is especially timely with the recent encounter of ESA’s Rosetta spacecraft with Comet 67P/Churyumov-Gerasimenko which ended in September 2016. Applications of SUISEI will be made to comets and the near-Sun object, (3200) Phaethon. - 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
5月24日（水）
- Campus
- Mitaka
- Seminar
- SOKENDAI colloquium
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- May 24 2017, 10:30-12:00
- Place
- Large Seminar Room
- Speaker1
- Kotomi Taniguch
- Affiliation
- SOKENDAI D3 (Supervisor; Masao Saito)
- Title
- Survey Observations in the 45 GHz and 90 GHz Bands toward High-Mass Star-Forming Regions
- Abstract
- We carried out survey observations of carbon-chain molecules and N2H+ in the 45 GHz and 90 GHz bands toward high-mass starless cores (HMSCs) and high-mass protostellar objects (HMPOs) with the Nobeyama 45-m radio telescope in the last two observational seasons. Our main purpose is to investigate the chemical evolution in the high-mass star-forming regions. We compare the I(N2H+)/I(HC3N) ratios using the 90 GHz band lines among HMSCs and HMPOs, and found that the ratios decrease from HMSCs to HMPOs, in contrast to the low-mass star-forming regions and giant molecular clouds. The column density of HC3N derived from 45 GHz line is well correlated with the integrated intensity of CCS, but that derived from 82 GHz line is not correlated. The high-excitation energy HC3N is enhanced in HMSCs where SiO has been detected. From these results, we propose that HC3N is re-generated in the shock regions driven by molecular outflows.
- Speaker2
- Misaki Ando
- Affiliation
- SOKENDAI D1 (Supervisor; Daisuke Iono)
- Title
- Molecular Gas Obsarvation in Local Merging U/LIRGs
- Facilitator
- -Name：Misaki Ando
- Comment
- TV conference system is available connecting from Nobeyama,
Hawaii, Mizusawa, and Okayama.
5月24日（水）
- Campus
- Mitaka
- Seminar
- DTA colloquium
Regularly Scheduled - Date and time
- 24 May 2017, 13:30-14:30
- Place
- Conference Room, Cosmos Lodge
- Speaker
- Naonori Sugiyama
- Affiliation
- IPMU
- Title
- Kinematic Sunyaev-Zel’dovich effect
- Abstract
- (optional)
Over the past few years, cosmologists have been able to make the first detections of the kinematic Snuyaev-Zel’dovich (kSZ) effect by combining galaxy data with measurements from CMB experiments. The kSZ effect is well-suited for studying properties of the optical depth of halos hosting galaxies or galaxy clusters. As the measured optical depth via the kSZ effect is insensitive to gas temperature and redshift, the kSZ effect can be used to detect ionized gas that is difficult to observe through its emission, so-called “missing baryons”. This work presents the first measurement of the kSZ effect in Fourier space. While the current analysis results in the kSZ signals with only evidence for a detection, the combination of future CMB and spectroscopic galaxy surveys should enable precision measurements. This talk emphasizes the potential scientific return from these future measurements. - Facilitator
- -Name：Tomoya Takiwaki
- Comment
- in English
5月26日（金）
- Campus
- Mitaka
- Seminar
- Solar and Space Plasma Seminar
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- 26 May (Fri), 13:30-15:00
- Place
- Student Seminar Room, Subaru Bldg.
- Speaker
- Masao Takata
- Affiliation
- Department of Astronomy, University of Tokyo
- Title
- Depressed dipolar modes of solar-like oscillations in red giant stars
- Abstract
- High-precision photometric observations from space by CoRoT and Kepler missions have recently detected solar-like oscillations in a large number of red giant stars. Study of the internal structure of these stars through the detailed analysis of their oscillation properties has accordingly been one of the hottest topics in asteroseismology. While there have been some important achievements, including the internal rotation profiles and the discrimination of the hydrogen-shell-burning and helium-core-burning phases, there exits an unresolved problem in the red giant seismology, which is known as the problem of depressed dipolar modes. In about 20% of the red giant stars with the solar-like oscillations, the amplitude of the dipolar modes, which have anti-symmetric oscillation patterns with respect to the equatorial plane, is considerably smaller than that of the radial modes, which correspond to spherically symmetric oscillations, in the same frequency range (Mosser et al. 2012). This is an unexpected result because the standard picture of the stochastic excitation of the solar-like oscillations by the near-surface turbulent convection predicts similar (or even higher) amplitude of the dipolar modes. In this presentation, this problem and its possible solutions are discussed in detail. A particular attention is paid to an idea of resolving the problem by the presence of the magnetic field in the helium core, which is recently proposed by Fuller et al. (2015).
- Facilitator
- -Name：Shin Toriumi
- Comment
-
—
Shin Toriumi, Ph.D.
Solar and Plasma Astrophysics Division
National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan shin.toriumi@nao.ac.jp
5月26日（金）
- キャンパス
- 三鷹
- セミナー名
- 国立天文台談話会
- 定例・臨時の別
- 定例
- 日時
- 5月26日（金） 16:00-17:00
- 場所
- 大セミナー室
- 講演者
- 広海健
- 所属
- 国立遺伝学研究所
- タイトル
- 研究プレゼンテーションのなぞ ～聴衆エネルギーと聴衆マター～
- Abstract
-
研究プレゼンテーションは研究者にとって必須の活動の一つです。プレゼンの出来で研究の進展やキャリアが左右されることもよくあります。みなさんも、学会発表、プログレスレポート、あるいはジョブトークなど多くのプレゼンをされているでしょう。でもその際に、以下のような疑問を抱いたことはないでしょうか？
・なぜ質問がでないのか？
・なぜ聴衆は寝るのか？
・なぜ職が得られないのか？
私自身も長年こういう疑問を持ち続けてきました。このような疑問に答え、研究者のキャリア活動を支援するために、国立遺伝学研究所（遺伝研）では英語プレゼンテーションのカリキュラム「遺伝研メソッド (NIG Method)」を開発しました。英語表現の技術向上だけでなく、論理的思考力や議論する力も培える方法論ですので、ポスドクや教員にも好評です。今回のセミナーでは、研究プレゼン能力向上に役立つコンセプトとして「聴衆エネルギー」と「聴衆マター」を紹介します．これらは「聴衆の特性の一部」であり、「発表言語に依存しない」ことは意識されていたものの、その実体はなぞでした。「聴衆エネルギー」と「聴衆マター」を定性的・定量的に理解してプレゼンテーションの組み立てに利用することで、疑問の解消に挑みます。このセミナーが天文科学分野に「遺伝研メソッド」を導入する契機になれば幸いです。 - 連絡先
- -名前：松田 有一
以上