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2018.05.28-06.03

5月29日(火)13:30~14:30   理論コロキウム            講義室  
May 29 Tue          DTA colloquium          Lecture room 

5月29日(火)13:30~15:00  太陽系小天体セミナー         南棟2階会議室  
May 29 Tue      Solar System Minor Body Seminar  Conference Room, South Bldg.2F

5月30日(水)10:30~12:00  総研大コロキウム           講義室
May 30 Wed        SOKENDAI colloquium      Lecture Room

6月1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   
Jun 1 Fri       Solar and Space Plasma Seminar  Student Seminar Room, Subaru Bldg. 

6月1日(金)16:00~17:00   国立天文台談話会         大セミナー室  
Jun 1 Fri           NAOJ Seminar        Large Seminar Room 

詳細は以下をご覧下さい。

5月29日(火)

Campus
Mitaka
Seminar
DTA colloquium
Regularly Scheduled/Sporadic
Regularly Scheduled
Date and time
May 29, 2018, 13:30-14:30
Place
Lecture room
Speaker
ShingChi Leung
Affiliation
IPMU
Title
Pulsation Pair-instability Supernova: Connection to massive black hole, circumstellar medium and collapsar

Abstract
Pulsation Pair-instability Supernova (PPISN), unlike its less massive relative core collapse supernova (CCSN) or more massive relative pair-instability supernova (PISN), pulsates with a large amplitude and experiences significant mass loss before its collapse into a black hole. It is a robust candidate of massive black holes (30 – 50 solar mass) as deduced by the gravitational wave signals detected by LIGO and Virgo.
It is also one of the source for the super-luminous supernova in the interaction framework.
Therefore, PPISN has an important role in the recent development of astronomy. In this talk, I will cover our recent PPISN project which follows the evolution of PPISN from its He-burning phase until its collapse using the MESA (Modules for Experiments in Stellar Astrophysics) code. I will discuss the diversity of mass loss, its final remnant and pre-collapse observable in the family of PPISN. Then I will discuss the implications of PPISN on the current mass distribution of massive black hole, on the features of super-luminous supernovae and on the formation of collapsar.

Facilitator
-Name:Tomoya Takiwaki
Comment
in English

5月29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29日(火曜日)13時30分~15時
場所
南棟2階会議室
講演者
渡部潤一

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30日(水)

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

Place
Lecture Room

Speaker
Yongming Liang
Affiliation
SOKENDAI 1st year (M1)(Supervisor: Nobunari Kashikawa (U.Tokyo),Masayuki Tanaka,Yuichi Matsuda)
Title
Search for massive overdensities at z~2.2 with Subaru HSC
Abstract (if you like):

Speaker
Masaki Yoshida
Affiliation
SOKENDAI 4th year (D2)(Supervisor: Yoshinori Suematsu,Hirohisa Hara,Ryohko Ishikawa)
Title
Wave-front error measurements and optical alignment of CLASP2 telescope
Abstract (if you like):

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.

6月1日(金)

Campus
Mitaka
Seminar
Solar and Space Plasma Seminar
Regularly Scheduled/Sporadic
Regular
Date and time
1 June (Fri), 13:30-15:00
Place
Student Seminar Room, Subaru Bldg.
Speaker
Shoko Miyake
Affiliation
National Institute of Technology, Ibaraki College
Title
Cosmic ray modulation and radiation dose at a flight altitude in the past 30 years and in the near future
Abstract
The Sun is exhibiting low solar activity levels since the descending phase of the solar cycle 23, and it is likely to be continued as well as in the case of the past grand solar minima. It is well known that the variation of the galactic cosmic rays (GCRs) spectrum below a few 10 GeV is caused by the heliospheric environmental changes. This variation, the so-called cosmic ray (CR) modulation, shows basically an anti-correlation with solar activity with an 11 years periodicity. In the current weak solar cycle, we expect that the flux of GCRs is getting higher than that in the previous solar cycles, leading to the increase in the radiation exposure in the space and atmosphere. In order to quantitatively evaluate the possible CR modulation and resultant radiation exposure at a flight altitude in near the future, we have developed the time-dependent and three-dimensional model of the CR modulation.
Our model can give the flux of GCRs anywhere in the heliosphere by considering the variation of the solar wind velocity, the strength of the interplanetary magnetic field, and its tilt angle. We solve the curvature and gradient drift motion of GCRs in the heliospheric magnetic field, and therefore reproduce the 22-year variation of the CR modulation without discrepancy with the flux of GCR protons observed by BESS and PAMELA. We also calculate the neutron monitor counting rate and the radiation dose of aircrews at flight altitude, by the air-shower simulation performed by PHITS (Particle and Heavy Ion Transport code System).
In this talk, I will present our recent works performing quantitative predictions of the CR modulation and the radiation dose at a flight altitude up to 2030.

Facilitator
-Name:Shin Toriumi

Comment

6月1日(金)

Campus
Mitaka
Seminar
NAOJ seminar
Regularly Scheduled/Sporadic
Scheduled
Date and time
Fri 1 June. 16:00-17:00
Place
Large Seminar Room
Speaker
John O’Meara
Affiliation
St. Michael’s College
Title
” Telling the Story of Life in the Universe: The LUVOIR Mission Concept”
Abstract
To tell the full story of life in the universe requires a space
telescope that is both extremely powerful and flexible. In this talk,
I will describe just such a telescope: LUVOIR, the Large Ultraviolet
Optical InfraRed Surveyor.
LUVOIR is one of four large mission concepts for which the NASA
Astrophysics Division has commissioned studies by Science and
Technology Definition Teams (STDTs) drawn from the astronomical
community. We are currently developing two architectures: Architecture
A with a 15.1 meter segmented primary mirror, and Architecture B with
a 9.2 meter segmented primary mirror. LUVOIR will operate at the
Sun-Earth L2 point. It will be designed to support a broad range of
astrophysics and exoplanet studies. The initial instruments developed
for LUVOIR Architecture A include 1) a high-performance optical/NIR
coronagraph with imaging and spectroscopic capability, 2) a UV imager
and spectrograph with high spectral resolution and multi- object
capability, 3) a high-definition wide-field optical/NIR camera, and 4)
a high resolution UV/optical spectropolarimeter. LUVOIR will be
designed for extreme stability to support unprecedented spatial
resolution and coronagraphy. It is intended to be a long-lifetime
facility that is both serviceable, upgradable, and primarily driven by
guest observer science programs. I will describe the observatory, its
instruments, and survey the transformative science LUVOIR can
accomplish, and I will extend an invitation to contribute science
programs to our program.

Facilitator
-Name: Matsuda, Yuichi

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