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2017.10.2-10.8

10月3日(火)13:30~14:30   理論コロキウム                 コスモス会館会議室
Oct 3 tue              DTA colloquium                Conference Room, Cosmos Lodge

10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
Oct 3 tue              Solar System Minor Body Seminar    Conference Room, South Bldg.2F

10月4日(水)10:30~12:00   総研大コロキウム                講義室
Oct 4 wed             SOKENDAI colloquium            Lecture Room

10月4日(水)13:30~14:30   理論コロキウム                 コスモス会館会議室
Oct 4 wed              DTA colloquium                Conference Room, Cosmos Lodge

10月6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
Oct 6 fri               Solar and Space Plasma Seminar     Student Seminar Room, Subaru Bldg.

10月6日(金)16:00~17:00   国立天文台談話会                大セミナー室
Oct 6 fri               NAOJ Seminar                  Large Seminar Room

詳細は以下をご覧下さい。

10月3日(火)

Campus
Mitaka
Seminar
DTA colloquium
Regularly Sporadic: Sporadic
Date and time
Oct. 3, 2017, 13:30-14:30
Place
Conference Room, Cosmos Lodge
Speaker
Matthew Kenworthy
Affiliation
Leiden Observatory
Title
Looking for exorings towards Beta Pictoris, J1407 and PDS 110
Abstract
Circumplanetary disks are part of the planet and moon formation process, passing from an optically thick regime of gas and dust through to a planet with retinue of moons and Roche lobe rings formed from the accreted material. There should therefore be a transitional phase where moons are beginning to form and these will clear out lanes in the circumplanetary disk, producing Hill sphere filling ‘rings’ hundreds of times larger than Saturn’s rings. We have seen evidence of these objects transiting their young star – with J1407, and more recently, with the young star PDS 110. This star shows periodic eclipses lasting over two weeks of up to 30% in depth, and the next eclipse is predicted to occur in September this year. The star is 10th magnitude in the belt of Orion, and can be followed in the early morning skies from most places on Earth. We are also following the Hill sphere transit of Beta Pictoris b, a gas giant planet around a nearby bright star, and I will also present the latest light curves from this experiment
Facilitator
-Name:Tomoya Takiwaki

Comment
in English

10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
10月3日(火曜日)13時30分~15時
場所
南棟2階会議室
講演者
佐藤幹哉

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

10月4日(水)

Campus
Mitaka
Seminar
SOKENDAI colloquium
Regularly Scheduled/Sporadic
Regular
Date and time
October 4 2017, 10:30 -12:00
Place
Lecture Room

Speaker1
Koki Okutomi
Affiliation
SOKENDAI D3 (Supervisor; Yoichi Aso, Raffaele Flaminio, Ryutaro Takahashi)
Title
Control Optimization for Vibration Isolation Systems in KAGRA

Speaker2
Satoshi Tanioka
Affiliation
SOKENDAI M2 (Supervisor; Yoichi Aso)
Title
The Dawn of Gravitational Wave Astronomy
Abstract
Advanced LIGO detected a gravitational wave signal produced by the coalescence of binary black holes during the second observing run (O2). From this result, what we can learn?

Facilitator
-Name:Misaki Ando

Comment
TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.

10月4日(水)

Campus
Mitaka
Seminar
DTA colloquium
Regularly Scheduled
Date and time
Oct. 4 2017, 13:30-14:30
Place
Conference Room, Cosmos Lodge
Speaker
Yuri Aikawa
Affiliation
Dept. Astronomy, University of Tokyo
Title
Deuterium Fractionation in Protoplanetary Disks
Abstract
(optional)
Deuterium enrichments in molecules are found in star-forming regions, as well as in Earth’s ocean. Asrtrochemical models show that the enrichment originates in exothermic exchange reactions at low temperatures, which could proceed not only in molecular clouds, but also in the cold regions of protoplanetary disks. In recent years, several groups observed deuterated molecules in disks using ALMA, in order to investigate the significance and spatial distribution of the fractionation. Brightness distributions of deuterated molecular lines vary with species and objects. In TW Hya, DCN is centrally peaked, while DCO+ is offset from the center, which suggests that they are formed via different deuteration paths. In AS 209, on the other hand, DCO+ and DCN emissions show similar distribution. Motivated by these observations, we calculate the reaction network model of deuterium chemistry in protoplanetary disks. Our model includes various deuterated molecules, exchange reactions, and nuclear spin-state chemistry of H2 and H3+, which affects the efficiency of deuterium enrichment. We found that the exchange reaction responsible for the fractionation varies among regions. While the exchange reactions of HD with H3+ and CH3+ are effective, as expected, the exchange reaction of D atom with HCO+ is also found to be important in warm regions and disk surface. As long as cosmic rays penetrate the disk, ortho/para ratio of H2 is found to be almost thermal, which lowers the efficiency of fractionation via CH2D+ compared with previous models which assume that H2 is all in para state. We also discuss the effects of grain size and turbulent mixing on deuterium chemistry.
Facilitator
-Name:Tomoya Takiwaki

Comment
in English

10月6日(金)

Campus
Mitaka
Seminar
Solar and Space Plasma Seminar
Regularly Scheduled/Sporadic
Regular
Date and time
6 October (Fri), 13:30-15:00
Place
Student Seminar Room, Subaru Bldg.
Speaker
Tomoki Kimura
Affiliation
RIKEN
Title
Transient brightening of Jupiter’s aurora observed by the Hisaki satellite and Hubble Space Telescope during approach phase of the Juno spacecraft
Abstract
In early 2014, continuous monitoring with the Hisaki satellite discovered transient auroral emission at Jupiter during a period when the solar wind was relatively quiet for a few days. Simultaneous imaging made by the Hubble Space Telescope (HST) suggested that the transient aurora is associated with a global magnetospheric disturbance that spans from the inner to outer magnetosphere. However, the temporal and spatial evolutions of the magnetospheric disturbance were not resolved because of the lack of continuous monitoring of the transient aurora simultaneously with the imaging. Here we report the coordinated observation of the aurora and plasma torus made by Hisaki and HST during the approach phase of the Juno spacecraft in mid-2016. On day 142, Hisaki detected a transient aurora with a maximum total H2 emission power of ~8.5 TW. The simultaneous HST imaging was indicative of a large ‘dawn storm’, which is associated with tail reconnection, at the onset of the transient aurora. The outer emission, which is associated with hot plasma injection in the inner magnetosphere, followed the dawn storm within less than two Jupiter rotations. The monitoring of the torus with Hisaki indicated that the hot plasma population increased in the torus during the transient aurora. These results imply that the magnetospheric disturbance is initiated via the tail reconnection and rapidly expands toward the inner magnetosphere, followed by the hot plasma injection reaching the plasma torus. This corresponds to the radially inward transport of the plasma and/or energy from the outer to the inner magnetosphere.
Geophysical Research Letters, Special Issue Early Results: Juno at Jupiter 10.1002/2017GL072912

Facilitator
-Name:Shin Toriumi

Comment

10月6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
10月6日(金) 16:00-17:00
場所
大セミナー室
講演者
吉戸 智明
所属
筑波大学計算科学研究センター
タイトル
学術広報はどこへいくのか
Abstract
「広報は大事」。大学・研究機関や国家プロジェクトの運営でよく聞かれる言葉である。ところが、この言葉を発している人々の多くは広報の専門
家ではない。広報専任職員は徐々に増えているが、絶対数は少なく、組織運営に関わる例はまれである。専門家不在のまま広報の意思決定がされる
学術の世界。科学コミュニケーション、アウトリーチなどよく似た活動があるなか、広報はどんな存在と考えられていて、今後どこへ向かうのだろ
うか。

連絡先
-名前:滝脇 知也

以上

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