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2018.10.15-10.21

10月16日(火)13:30~15:00  太陽系小天体セミナー   南棟2階会議室   
Oct 16 Tue       Solar System Minor Body Seminar  Conference Room, South Bldg.2F

10月16日(火)14:30~15:30   理論コロキウム      講義室 
Oct 16 Tue          DTA colloquium        Lecture room

10月17日(水)10:30~12:00  総研大コロキウム      講義室 
Oct 17 Wed          SOKENDAI colloquium     Lecture room 

詳細は以下をご覧下さい。

10月16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16日(火曜日)13時30分~15時
場所
南棟2階会議室
講演者
土屋智恵

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16日(火)

Campus
Mitaka
Seminar
DTA colloquium
Regularly Scheduled/Sporadic
Regularly Scheduled
Date and time
Oct. 16, 2018, 14:30-15:30
Place
Lecture room
Speaker
Kazunari Iwasaki
Affiliation
Osaka University
Title
The formation of molecular clouds by compression of atomic gases
Abstract
The formation of molecular clouds is one of the fundamental building blocks
in star formation. In order to determine the initial condition of the star formation,
it is crucial to reveal the formation and evolution processes of molecular clouds.
We investigate the formation of molecular clouds from atomic gas by using
three-dimensional magnetohydrodynamical simulations including non-equilibrium
chemical reactions and heating/cooling processes. We consider super-Alfvenic
head-on colliding flows of the atomic gas possessing the two-phase structure.
We examine how the molecular cloud formation changes depending on the angle
between the upstream flow and mean magnetic field. If the atomic gas is
compressed almost along the mean magnetic field, the accretion of the highly
inhomogeneous upstream atomic gas drives a super-Alfvenic velocity dispersion
which decreases the mean density of the post-shock layer. Even a small obliqueness
of the magnetic field weakens the post-shock turbulence. As a result, the post-shock
layer becomes denser than that formed by a colliding flow almost aligned to
the magnetic field. If the magnetic field is further inclined to the upstream flow,
the shock-amplified magnetic pressure suppresses gas compression,
leading to an extended post-shock layer. Our results, therefore, show that
there is a critical angle which maximizes the mean density of the post-shock layers.
Developing an analytic model and performing a parameter survey, we derive
an analytic formula of the critical angle as a function of the mean density,
collision speed, and field strength of the upstream atomic gas. We also found that
the dependence of the post-shock layers on the angle causes a diversity of
the physical properties of dense clumps.

Facilitator
-Name:Tomoya Takiwaki
Comment
In English

10月17日(水)

Campus
Mitaka
Seminar
SOKENDAI colloquium
Regularly Scheduled/Sporadic
Regular
Date and time
October 17, 2018, 10:30 -12:00

Place
Lecture Room

Speaker
Satoshi Tanioka
Affiliation
SOKENDAI 3rd year (D1)(Supervisor: Yoichi Aso,R. Flaminio,T. Akutsu)
Title
Toward O3
Abstract
Advanced LIGO and Advanced VIRGO will start 3rd observing run from early 2019. KAGRA is trying to join this observing run. I will report on the current status of KAGRA.

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.

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