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硼ȥ2014

硼ȥΥߥʡǤꡢ§Ȥ轵θ13:30鳫ŤƤޤ

Schedule & History

2010ǯ 2011ǯ 2012ǯ 2013ǯ

Abstract

4/23ƣ̻() ̴ؿΤĤΥץ
Ĥ˼̴ؿ硢Ƥ̤ξ١ĤΥץ֤ûʤ뤳ȤΤƤ롣ܸǤϡNΥߥ졼顢̴ؿĤΥץ֤ɤΤ褦˷ޤäƤΤĴ٤η̡γҿ¿ޤϼ̴ؿμ椬硢ĤΥץ֤ϺǤŤϳŪ໤Ĥ濴ॿॹȤʤꡢ̤ȿ㤷ûʤ뤳Ȥ狼äޤ椬礭ϡ¼Ū˾γҷϤƱͤʿʲ򤷡ץȤݤʤȤ狼ä
5/7(CfCA)ȥŷΤǮʲ
õϤ֤ȥ狼äγҤδѻ̤顢餬и٤䤽ǯʤɤ狼äǡΤ褦ʴĶã뤿ˤϥȥŷΤϤɤΤ褦ŷΤǤäõ뤳ȤŪȤԤäͷ׻̤饤ȥŷΤΥ䤽ηǯäǤΤǡξҲԤ
5/14ӹ(/)֥åۡоιή׳Ψ˵Ǥδ¬Ūħ
֥åۡεоιήоˤơ¬ϤФе̤ǰƬ֤Ƥ뤬¬ԤˤȤäƸŪ1ˤʤ̤ϰ̤ˤϵˤϤ餺äŪήˤƤϡ̤礭뤳ȤŦƤ롣 οǯˤ錄ꡢȤռͰˤäƸŪ˸оᤤƤˤĤơŪŪߤ򤭤ȹθơ¬ŪˤɤΤ褦ħ򼨤ƤȹռͤȤ礭졢٤跿ڥȥˤʤ뤳Ȥʤɤ򼨤Ū˸оιήǤϡ̹Ψ׳Ψ꽽ʬ礭С̤Ͻʬ˰֤뤿ᡢ®٤⾮ޤ礭ʰ㤤Ϥߤʤͽۤ줿 ̹Ψ׳Ψ˵Ǥϡθ̤Ͼʤꡢ®٤礭ʤΤǡṲ̄ƯƤȹͤ롣 ܸǤ׳Ψ˵εоιή˹ʤäơθ׻оιήδ¬ŪħĴ٤̤𤹤롣
5/21ư(CfCA)¿ߡʬˡ
ߡʬˡޤᡢͷϤϳؿʲĴ٤뤿ˤ褯ȤƤʬˡǤ롣ߡˡϥץ쥯ƥåʬˡȰۤʤꡢͥ륮֤˰¸ĹƤޤĹַ׻ԤݤˤϸѤ߾夬äƤޤ꤬롣ǡߡʬˡ¿ŬѤĹ֤η׻ǤޤˡξҲԤ
5/28ⶶǷ(CfCA)R2MHDɤˤĶ׳פŪͼ¸GR-RMHDɳȯ
֥åۡ(BH)Ϲ٤ξʤΤ濴¸ߤ褦ʵBH¸ߤɤΤ褦BHĹ̤Ǥ롣桹Υ롼פǤϥˤ BHĹǽǤ뤫Ĵ٤뤿R2MHDɤѤŪͼ¸Ԥäη̡BHؤμ̹ΨФŵŪʾ(륨ǥȥΨˤ¸ߤBHεĹϲǽǤ狼äη׻Ǥ(i)˽ʬʥ뤳ȡ(ii)Ṳ̵̄ǤȤ꤬äƤä˸ԤˤĤƤϥ֥åۡ뤬žƤ˸ˤʤǽ롣Ǽ˲桹R2MHDɤȯŸGR-RMHDɤȯξܺ٤ˤĤƤ𤹤롣
6/4()ȯŷΥ٥ˤextremely radio-loud AGNȯ
ǯĶȯʤɤõ뤿¿ȯŷΥ٥¬ԤƤ롣¿Ķȯưॹ˹碌ơƱδ¬ԤäƤ뤿ᡢ1ʲΥॹưŷΤθ̤ΰǤ롣1ɤۤ뤿ᡢ桹ϡ¬Υߥå˾ѤƹȯŷΥ٥ԤäƤ롣Υ٥μŪϡĶȯξ׷Ȥɽ̤ãִ(å֥쥤)ª뤳ȤǤ뤬٤ȿ¬ԤȤˤ͡ŷΤûưݤª뤳ȤǤ롣ܥǤϡΥ٥Ƕȯ줿ûưAGNˤĤƾҲ𤹤롣
6/11̾()夤ϥ󥺸̤ǸФ줿ĤXͤ
Фϥ󥺥٥ˤäƸФ줿ĤζĤXեå״¬η̤ˤĤ𤹤롣ĤˤĤƤϡChandraˤ뿷ʴ¬ԤĤΣĤˤĤƤϡChandraXMM-NewtonΥ֥ǡѤϥ󥺶ĤX٤X٤δطϡXǸФ줿ĤΥ󥰴طƱͤǤäX٤ȶļ̤δطˤĤƤϿ㤤줿ο㤤ϡϥ󥺤ˤ¬ΥХθȷڸ롣ޤXѤƶĤϳع¤ꤷϳع¤ΰ㤤ˤ륹󥰴طؤαƶƤ̤𤹤롣
6/18(CfCA)Ķȯοѥ
ޤĶθԤϡɸ¤ǤȯƤĶߥ졼ȯʤɤȤβܻؤƤ˥塼ȥΤǸγ¦Ǯ륷ʥꥪͤȤηоΤ˲ꤷߥ졼ǤϡĶȯʤΤǤ롣 ξ϶ǯɥ饹ƥåѤꡢ¿ߥ졼ˤȯǥ뤬ϤƤ롣ߥ졼Ǥή߹׷԰ʤɡ ʪ¤̤˼졢餬˥塼ȥβǮ¥ʤ뤳Ȥ ǽŪȯ뤳ȤʬäƤ ĶϲȤ櫓ǤϤʤ¿ߥ졼Ǥϡ꤮ȯƤ뤿ᡢʪΤäȤ㤤ǡȯʤȤ⤢ΤǤ롣 ϹͤƤʪ򥢥åץǡȤ¿ߥ졼ԤĶȯꤵɬפ줬ĶȯοѥǤ롣 ܥߥʡǤϡˤṲ̄ȡĶȯβ˸ɥޥåפ򼨤
6/25ٺ幬()եȾϳʿղ
ʬұܷ֤֥եȡפǤȤѥबϡδ¬̤Ʒ褦ˤʤäиδ¬եȤӤϥեȤ˿ľǤȹͤƤ롣Τ褦ʥեȤΥϡǮϡϡܳ礤ϳʿղĴ٤Ƥ뤬ϡ«ФƼ̤ɤΤ褦ʬۤƤ뤫mass loadingˤʿղˤɤΤΤĴ٤̤Ҥ٤롣Υ塼ǤϤä׻ˡˤĤƤҤ٤롣
7/2ʿͪ(/)侮Ϥβưϳؿʲߥ졼󤫤õrץεŷ
Ф˾VLT緿˾Ѥʬʬ¬ˤäơǯϷϵڤӤμ¸ߤ侮ινŸξܺ٤餫ˤĤĤ롣ˤŸǤζʬۡʬۤϡϤϳؿʲͳ褹ˤȿǤϤǤꡢؿʲϳؿʲƱ˷׻뤳ȤˤäƽǤΤȤơܤϤƤ롣ǤϡäĶȯϢϤιΤʤɤȯݤǹȹͤƤrץǤܤ롣Ƕθǹ׻ˤȡ˥塼ȥβǮĶȯǤϡ̿礭rץǤΤ񤷤ȤƤ롣ϢϤιΤǤϡΤޤǤ˰첯ǯ٤פȡ[Fe/H] < -2.5 ǹ⤤[Eu/Fe]ǤʤȤ꤬ŦƤ롣ǡ桹ϡN/Smoothed Particle Hydrodynamics ɤĶȯΤȼͥ륮ȽŸǤΥեɥХåθ̤줿ϳؿʲǥۤơ˼ȤǤ롣ܥǤϡrץǤοʲޤ᤿ϳؿʲǥҲ𤷡侮ϤˤĤƹԤäϳؿʲ׻η̤ˤĤ𤹤롣
7/9ƣů()ήʬұˤ뼫ʽϼ̥η
줬ʬұˤȤȡޤǤפ֤¬ͽۤĹ᤮뤳ȤŦƤθ塢ʬұˡʴ¬Ƥ褦ʡ礭ή®٤ľ硢줬Ƥη֤ûʤͥߥ졼ˤäƼ줿֤ûʤᥫ˥ŪƤϤʤäǡǤϤΥᥫ˥ˤĤƹͻη̡ޤǤλ֤®٤δؿȤɽŪʳμʤȤƳФʪˤˤꡢ褽ͥߥ졼η̤뤳ȤǤ
7/16ݱѰϺ()ϵ巿η
Ƕι٥ɥåץ顼ˡȥ󥸥åˡˤäơ¿ιζ˵ϵ巿()ȯƤ롣ΤۤȤɤʣϤ¸ߤƻ̤ϤۤܤäƤƵƻΥΨϾ۷ϵ巿Ӥơƻֳ֤Τ褦Ϥη¿Υߥ졼ˤäĴ٤Ƥ롣϶ϵ巿κǽʳǤͤδʪ۷ϵ巿εͤӤʤҲ𤹤롣
7/23 Benjamin Wu (University of Florida)GMC Collisions as Triggers of Star Formation
We utilize magnetohydrodynamic (MHD) simulations with adaptive mesh refinement (AMR) to explore the process of GMC-GMC collisions as a potential trigger for star formation. We start by implementing new PyPDR/Cloudy-based density/temperature/extinction-dependent heating and cooling functions in Enzo that span the atomic to molecular transition and can return detailed diagnostic information. We then explore a suite of idealized 2D simulations for GMC-GMC collisions, which track the fate of an initially stable clump embedded within one of the clouds. Different collision velocities, impact parameters, magnetic field strengths and orientations are considered, as is the role of ambipolar diffusion. We determine the ability of cloud collisions to compress the clump and perhaps initiate its global collapse. We then extend these calculations to 3D, including introduction of initial turbulence into the clouds. Filament creation and interaction is visualized and analyzed. We discuss potential diagnostic signatures of GMC collisions and compare to some proposed example cases in the Galaxy.
10/01ë()ͣȣĥꥳͥˤ밵ήθ
ۥʡϵ弧뤤Ϲ⥨ͥ륮ŷδĶǤϡ >> ץ饺ްϤ¥ץ饺ǡꥳͥ󤬵Ƥ롣´ĶǤΣͣȣĥꥳͥϡĹǯˤ錄äƸ椵ƤơޤǤ뤬ǶᡢŪʥߥ졼ˡƳȤȤ˿¦̤Ƥ㤨СZenitani & Miyoshi (2011) ϡץ饺ޤݤ줿ץ饺⥤ɡʼ˼դ˿׷ȹ¤Ǥ뤳Ȥ𤷤Ƥ롣 ȯɽǤϡη̤򾯤㤦ʰήϳء®ήϳءˤǺƹͤ롣 ήϳؤǤϡŵŪή®٤®Ʊ٤ˤʤȡޤޤʰήθ̤롣Ϥޤ˥åȤŵ®٤®Ķ¥ꥳͥˤƤϤޤꡢҶ̤˸׷Ȥ䡢ХΥǤǮ®ȤäήθݤƤ롣äˡĶ®åȤ˸֥åɡפȤݤܤ׳и䡢ϷϳåȤʪȤζ롣
10/08¼()Ultra Fast OutflowΥ饤եưǥ
ưϳ(AGN)ռͥڥȥаܤۼȯ졢åȤȤϰۤʤ륢ȥե뤳Ȥ狼äƤäUltra Fast Outflow (UFO)ȸƤФ륢ȥեSeyfertϤȾǴ¬Ƥꡢ®٤Ψ礭Ȥ֥åۡĹϤˤƶƤǽ롣ȥեΤϹɽ̤ʮФǤȹͤƤ뤬ʮХᥫ˥乽¤Ǥ롣桹ͭϤʥǥΰĤǤ饤եưռήΥߥ졼Ԥä׻η̡Ѥ礭®٤®10ãʮФΥ٤®١̩٤UFOX¬鼨ͤȰפ˥֥å̤ۡ䥨ǥȥʤɤѤƥߥ졼Ԥä̡AGNǤϱȯquasarnarrow line Seyfert 1UFO¬ǽ뤳Ȥ狼äη̤˲äơߥ졼̤򸵤ˤռͥڥȥ׻ˤĤƤҲ𤹤롣
10/15ܲ()üŪռͼήϳط׻οˡ
ռ;ǡ򤯤ŷʸؤĹǯˤ錄äƤǤ롣θˤƤϡռ͢ʷ׻̤ޤ뤿ˡ⡼ˡѤŪʷ׻ˡѤƤŪߤŪ̩٤̩㤷ǤʤȤäDz桹ϡְ¸ռ͢򤭡ռ;ήΤƱ˻ȯŸ׻ˡȯϲζˡȤϼŪ˰ۤʤ뿷ʼˡǤ롣üϥեȤ߹ǤꡢŻһⰷ롣ˡ۲ˡ򹪤ߤȤ߹碌뤳Ȥ絬׻ǽǤ롣®ǥॹƥåפޤΤǡή٤ݤؤŬѤ󸽼ŪǤ뤬֥åۡϤθݤĴ٤Ǥ϶ˤͭѤʼˡǤ롣
10/22Ƴ()ϢΤˤץǹȳʬȿ
ץŴŤǤĤפʸǹǤ뤬줬ɤŷΤǵƤ뤫̤狼äƤʤǯοͥߥ졼󤫤ĶȯǤϣץʤȤƤ롣ϢιΤϤ˼äץŷΤȤܤƤ롣ϢΤǤΣץǤϡҿ̩٤⤤˳ʬ򤹤褦ʽŤҳˤĤ롣ΤᡢʬȿפʳȿΰĤˤʤ롣ȯɽǤϡʳʬǥѤϢΤθǹ׻ˤĤƵ롣
10/29Ľ()ץ쥯ƥåͲˡ
ץ쥯ƥåͲˡϥϥߥȥϤФѿͲˡǡʬβλȯŸץ쥯ƥåȸ̩¸ΥˡǤ롣ץ쥯ƥåͲˡǤϥͥ륮ɤ¸졢Ĺ֤οͷ׻ˤɬܤΤΤȤʤäƤ롣Υץ쥯ƥåͲˡδû (i) ץ쥯ƥåͲˡκ(ii) ͥ륮ͳȤĴ¿ưҤ롣
11/19ҵ()Υե¸ߤΤ
2012ǯKashinskyϡĤWMAPˤ뱧ޥط͡CMBˤ餮¬ǡˡ35h^-1 MpcεΥΥ졼ȥȥ饯ۤ륹200700 Mpc˰ͤж˻Ūեʥեˤ¸ߤǽ򸡽ФŪˤϥޥե졼󡢥ץ쥤ե졼λ餮뤤ϥޥСˤ̻ҤĤ顢Τ褦礭ʱ襹Υե¸ߤͽ¬롣桹ϹаIaĶ¬ȶϤơIaĶаܡΥǡUnion.2.1SDSS-IIIΩ˺ɾơեθФߤη̡Union.2.1ΥǡϤϹ⤤аz>0.05㤤аz<0.05Ǹߤ˰ۤʤե®٤η̤SDSSIIIǡβϤ餳̷θ뤳Ȥߤshort talkǤϡη̤𤹤롣
11/26ƣܷ˻()3D dynamics of collisionless magnetic reconnection
Mangetic reconnection is one of the key processes which release the magnetic field energy into plasma kinetic energy and drive explosive phenomena in collisionless plasmas. A number of observations in the Earth magnetosphere, laboratory experiments, and solar flares have suggested that the reconnection process is essentially three dimensional. However, the 3D model of magnetic reconneciton was poorly established yet, in part, because of limitation of the comupter resources. The current study focuses on plasma turbulence arising around the magnetic x-line by using the K, the state-of-the-art supercomputer of Japan. We show that the electromagnetic turbulence not only gives rise to the anomalous electric resistivity, but also controls the outflow jet structure in large (MHD) scale. The 3D outflow jets may explain the bursty plasma flows observed frequently in the Earth magnetotail.
12/03ž(CfCA)ϱפˤؤΥȥ꡼ߥ԰οͥߥ졼
ηϡ̤ɤΤ褦ʥᥫ˥Ƿ줿򤵤ƤʤߡηΥᥫ˥ΰĤȤͭ˾뤵ƤΤȥ꡼ߥ԰Ǥ롣ȤĹϱפ濴̤˥Ȥ¤ƥؤȡȤȥϤߤ񹳤ڤܤ礦ϸۤˤꥱץ顼®٤ʬ٤žΤǡȤ鸫ȸ뤳Ȥˤʤ롣ѱư̤򼺤äȤ濴롣ΰǥȤζ̩٤äȡѱư̤Фƴ礭ʤΤ®٤롣ƤȤ򽸤뤳Ȥˤäơ®٤롣Τ褦ˤƥȤǻŪ«뤳ȤˤäȤᥫ˥बͥߥ졼ˤ꼨줿ֱܹǤϡΥᥫ˥βٰ¸Ĵ١ºݤޤǥȤǻǽ򸡾ڤ롣
12/17ͺ(/)Ѥˤ븶μž
۷ϷɸॷʥꥪǤϡȤФ뾮ŷΤνѤˤäƷ롣礭ۤɶϤǼͤ˽ŪĹƤ˽ŪĹ򸶻ȤʣƱ٤θεƻֳ֤ݤäĹʳŪĹȤܸ֡ǤϡĹˤ롢εƻʲȽѤ򡢽¿η׻ѤƷ׻˽Ѥ뼫žѱư̤׻뤳Ȥǡž®٤伫žг(ʲž)Ĵ٤Ƥ롣ȤơۼȾ 1AU Υ󥰾˼ 10^23g 9000 γʬۤפ̩٤ӥǥ1.5ܤȤ󥰤ϡγҤ̤θΩ٤ˤʤ褦ˤˡץʤη׻Ԥä̡μžгѤŪʬۤž®٤ˤĤƤϡ̤äȶ˾ʤ¸ߤ줿¿η׻ 10^26gޤĹμž®٤ϡƱβμž٤1.5®ʤäž®٤μ̰¸ϡ¿ξ̤Ū˽Ѥ뤳ȤǡѤѱư̤Ǥä뤿롣ΰ¸ν̤礭ȼ夯ʤ롣ϡμ̤礭ʤʤ뤳ȤǡѤˤѱư̤Ǿäʤʤ뤿Ǥ롣ޤ̩()ȼž®()δ֤ˤϦ ^1/2δط롣ߤϱץθ׻ԤäƤ롣ˤꡢϤ®ʬޤ졢Ѥѱư̤ʤ뤳Ȥǡž®٤ʤ뷹줿ȯɽǤϰʾ˲äƻդפΥåפμžθ˱ƶڤܤǽˤĤƤ롣
1/7()°޼ˤǮŪ԰Ϥߥ졼
ߤζϤˤǮŪ԰HIʬұݤ˶ˤƽפ̤Ƥ롣ܸǤϤǮŪ԰ʪŪ°̴ĶϤΣߥ졼μˡDzϤη̡°̤طʻ糰ζ٤ˤäǮŪ԰ĹǤ׳Ķ¸ߤ뤳Ȥ餫ȤʤäޤǮŪ԰Ĺ̵ͭ°ɤΤ褦Ѥ뤫ˤĤƤ롣
1/14¼ʸδ()ͤˤķ
ȾϽĤǷʤǤϴñΤĤȤ֡ˡΤᡢĤɤ뤫뤳ȤνפʲǤ롣ʤ顢ķˤ̤β꤬¿ǶΥߥȥ֥ߥȤδ¬Ĥϥѡι̩٥ʥסˤ뤳ȤʬäƤΤ褦ʥɤΤ褦˷뤫ɤʬäƤʤɤΤ褦ķפ뤫뤿˲桹ϷϤޤäФȻפΰSerpens Southȴ¬Ԥäη̡ΰˤϷķפķΥפ뤳Ȥ狼äˡķפϥեȤξͤˤäƷ줿褦Ǥ뤳Ȥ⼨줿ƱΤξͤķͶȯ硢ɤΤ褦ʹ¤ɤΤ褦ˤƷ뤫Ĵ٤뤿ᡢ桹ϱͤοͥߥ졼Ԥäߥ졼󤫤飲Ĥαξͤǹ̩٥եȤ뤳Ȥ狼äƤSerpens SouthΰΤĤŪ˱ͤǤ褦Ǥ롣
1/28Ĺëɧ(CfCA)ϱפǤΥȤĹ˲ȽѤβǽ
ϱδХȤϾͻ˲濴ؤʤɤΤñʾ͹ΤǤޤĹǤʤȹͤƤ롣褹뤿ˡȤƱפν԰GIˤ䥹ȥ꡼ߥ԰SIˤʤɤˤ뽸ѤͤƤ뤬˴ؤθǤϥȤĹϤޤθƤʤäܸǤä˥ȤĹܤȤĹGISIήȯ륱ӥ󡦥إۥ԰βǽͿƶˤĤĴ٤
2/18(CfCA)̲᤬濴ιⲹήͿƶ
G2濴ܶᤷ̲ᤷƤ뤳Ȥ𤵤Ƥ롣塢̲˱ƶ뤫ͽۤ뤿ˤϡ̲᤬濴֥åۡؤιⲹήͿƶ餫ˤɬפ롣ǡϥ̲᤹ⲹήռѤθ3MHDߥ졼»ܤη̡ζ̲ᤫ5-10ǯƼ줬뤳Ȥ狼äȯɽǤϡȡXǤβǽˤĤƤ롣
2/18һ(CfCA)ͤȼƻгѤθ
Keplerˤ16δ¬ˤä2300Ĥŷ(Batalha et al., 2013)ȯƤ롣ˤʣʤϤ899Ĵޤޤ롣ʣϤ818Ĥhot-NeptuneʲΥΤߤʤϤ¸ߤʣϤΤۤȤɤϥѡʤϤǤ뤳Ȥ狼äƤ롣ʣϤϤȡŪʵƻгѤŵŪ1.0-2.2Ǥä(Fabrycky et al., 2014)ѡξǽѤ硢ηгѤϵʳǤѤˤäƷޤȹͤ롣Υ®٤ϻˤäæ®٤ޤǾ徺뤬æ®٤ͽۤ뷹гѤ5.4٤Ǥꡢ¬礭ΥΨϵʳǤξͤǸꤹ뤳Ȥ餫ˤʤäƤꡢƱͤ˷гѤͤǸꤹǽ롣ǡܸǤϾͤȼгѤθʳNη׻Ĵ٤ηгѤĴ٤ȡ͸ηгѤɬηгѤ礭ʪ꾮ʤ뤳Ȥ狼äޤѲŪդNη׻줿гѤϴ¬ȰפƤꡢϥѡΤξ콸ѤǴ¬줿ѡϤǤ뤳Ȥ򼨺Ƥ롣