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## RLE(2021NxȑO)

### _wRLEifqj

 2021N125i΁j16F3018F00 V cG iwj uPQXJ[Əd͂̔ŏɂU(1)NIeB̉v W͌^QCD̔ۓʂɋNCPĂBɑ΂āAVɃXJ[𓱓邱ƂŋCP@mĂBPeccei-Quinn(PQ)@\ƌĂ΂ĂB̃XJ[̓ANVIƌĂ΂ĂAVɓꂽU(1)PQΏ̐̎IȔjɔ암S[hXg[łBPQ@\@\邽߂ɂU(1)PQΏ̐xŐ藧ƂvBAd͂̔ۓʂU(1)PQΏ̐傫j鍀𐶂ݏoAPQ@\䖳ɂ\wEĂBU(1)NIeBƂB{uł́APQXJ[Əd͂̔ŏ𓱓邱ƂU(1)NIeBł邱ƂB܂A{͌^͉Fwi˗R̐𖞑Ct[VłAƂƂɂyB { wr܃LpX44K4405ƃIC

### _wRLEiFj

 2021N118i΁j16F3018F00 Oc G ikCwwj uQuest for realistic non-singular black-hole geometriesv 1968 NBardeen ٓ_ȂubNz[̋Ώ̃f񏥂ĈȗAكubNz[̃f͗lXȓeō\Ă܂B{Z~i[ł͐̃f畨IɑÓȂ̂Iʂ邽߂7̏ĂA炷ׂĂ𖞂f̍\݂܂B { IC

### _wRLEifqj

 2021N111i΁j16F3018F00 Xc iÉwj ulBootstrap@pʎqn̉́v ̕wɂ, l͂͌Ȃ̂ƂȂĂ. {uł,ʎq̌nɂ鐔l͂̐VȎ@ƂċߔN񏥂ꂽBootstrap@Љ. Bootstrap@͌ݕWIȐl͎@ł郂eJ@ɑ΂Ď̂悤ȗ_: 1) 𓾂邱Ƃoꍇ. 2) o\. 3) }CNJmjJATuɂMtԂ𒲂ׂ\. ,lBootstrap@ɂׂ͍, ɂĂЉ. { IC

### _wRLEiFj

 2021N1220ij16F3018F00 s o (Éw) u͒cΌƉF}CNgwitˎldɗh炬pÍGlM[̐Vؖ@v ͒cɂF}CNgwiˁiCMBj̎ÚA͒c̈ʒuɂqz̎ldɈٕɏ]āAΌMUBUꂽΌ̑肩瓾邱́uuldɁv́A傫ȃXP[̌nIȗh炬č\z@񋟂B̂悤ɂčč\ꂽnIȗh炬ɂė\CMB̋ǏIȎldɂCMBqɂ钼ڊϑʂƂr邱ƂŁARX~bNoAX̕s萫𒴂ÍGlM[CMBϑɂeXg\ɂȂ邱Ƃc_B { wr܃LpX43K4340ƃIC

### _wRLEifqj

 2021N1214i΁j17F1518F45 (GlM[팤@\) uG^OgEGgs[Ɠ_֐v G^OgEGgs[(EE)́AnԂ̗ʎqւ𑪂wẄłBɏ̗_ɂāAEE͂܂łɁAɎRꗝ_Ƌꗝ_̏ꍇd_IɒׂĂBEEIȊϑʂƋ̓IɊ֌WÂɂ́Aʂ̗̏_ɂEE͂邱ƂsłB̍uł͂܂ÄƂĔԂƂꍇEEɂāAʂ̗̏_ɓKp\ȉX̉͂ЉBāAEE̎vƎv镔AlXȉZq̂肱܂ꂽ_֐pĔۓIɕ\邱ƂB̌AX̌ʂʂ̕nɊg邽߂ɁAȐꍇEEA^A_֐̊Ԃɂ֌WčlB { IC

### _wRLEifqj

 2021N127i΁j16F3018F00 F_ mI iswbwj uEntanglement between two gravitating universesv We study two disjoint universes in an entangled pure state. When only one universe contains gravity, the path integral for the nth Rényi entropy includes a wormhole between the n copies of the gravitating universe, leading to a standard "island formula" for entanglement entropy consistent with unitarity of quantum information. When both universes contain gravity, gravitational corrections to this configuration lead to a violation of unitarity. However, the path integral is now dominated by a novel wormhole with 2n boundaries connecting replica copies of both universes. The analytic continuation of this contribution involves a quotient by Z_{n} replica symmetry, giving a cylinder connecting the two universes. When entanglement is large, this configuration has an effective description as a "swap wormhole", a geometry in which the boundaries of the two universes are glued together by a "swaperator". This description allows precise computation of a generalized entropy-like formula for entanglement entropy. The quantum extremal surface computing the entropy lives on the Lorentzian continuation of the cylinder/swap wormhole, which has a connected Cauchy slice stretching between the universes -- a realization of the ER=EPR idea. The new wormhole restores unitarity of quantum information. { IC

### _wRLEiFj

 2021N1130i΁j16F3018F00 cJ (w) ud͔gkwƒqv VɎc钆q́A̍\ł炫ƌ܂ĂȂB̓m̎iƂāAkwB{Z~i[ł́AȒPɒqɂd͔gkwAۂɒV̌nqɂK̉\ɂċc_B { IC

### _wRLEiFj

 2021N1116i΁j16F3018F00 Ό G (sw) uU(1)Q[WEqbOXfɂmg|WJ\gƏd́v U(1)Q[WEqbOXf̓g|WJ[Wʑ ƂẴ\giNielsen-Olesen stringjƂmĂD ffXJ[ƌnlƁCɁCۑ[WƂ Ă̓dׂmg|WJȃ\glɑ݂邱Ƃ킩 D̃mg|WJ\g̐ƁCƂd͂ ċc_ { IC

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 2021N119i΁j16F3018F00 ׌ iJuAgF@\j uMatching higher symmetries across Intriligator-Seiberg dualityv 4 so QCD ́AJ[ƃt[o[Ƃɋ̏ꍇAʏ (0-form) Ώ̐ɉ "" (1-form) Ώ̐L邪A2̑Ώ͕̐K݂ɓƗłƂ͌炸AQ[WQ̑Iȍ\EJ[Et[o[Eg|WJȂǂɉāAAm}[ 2-group Ώ̐ƌĂ΂\ȂĂ肷B{uł́AΏ̐m̔񎩖Ȋ֌WɂĉAɒΏ QCD ̏ꍇɂ炪 Intriligator-Seiberg oΐ̉ŐIɈڂ荇ƂB { IC

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 2021N1026i΁j16F3018F00 D (Bw) uIndirect detection of gravitons through quantum entanglementv Fɗʎqh炬璼ڐ錴nd͔g̗ʎq(Or g)ϑ@ƂāAÎ̗ʎqfRq[Xϑ邱 ŁAOrgԐړIɌoł邱ƂĂ܂B̉ߒŁAOr gCt[VɃXNC[YԂɂȂ邱ƂɂăOrg ւ債ǍʁAOrgNÎ̗ʎqfRq[ X̋Cqɂ̂葁N邱Ƃ܂B { IC

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 2021N1019i΁j16F3018F00 isw@bwj uJT Gravity Limit of Liouville CFT and Matrix Modelv In this talk, we study a connection between Jackiw-Teitelboim (JT) gravity on two-dimensional anti de-Sitter spaces and a semiclassical limit of c < 1 two-dimensional string theory. The world-sheet theory of the latter consists of a space-like Liouville CFT coupled to a non-rational CFT defined by a time-like Liouville CFT. We show that their actions, disk partition functions and annulus amplitudes perfectly agree with each other, where the presence of boundary terms plays a crucial role. We also reproduce the boundary Schwarzian theory from the Liouville theory description. Finally, we identify a matrix model dual of our two-dimensional string theory with a specific time-dependent background in c=1 matrix quantum mechanics. { IC

### _wRLEiFj

 2021N105i΁j16F3018F00 M Ďj (sw bw) uR[h_[N}^[DF̔\v ͕z͒cȂǂ̊ϑŌ鎿ʕz̔ĺAnx炬R[h_[N}^[(CDM)ɂd͕s萫ɂĐAƍlĂBCDMDF̍\ʓIɋLq邱ƂŁAϑAn炬̏𖾂炩ɂAF_p[^[𐸖Ɍ肷ȊOɁA_[N}^[̐̂ɔ邱Ƃ\ƂȂB{Z~i[ł́Aۓ_ƃV~[VƂ̔rʂāAd͔i񂾍\̒ʋLqɊւŋ߂̐iWɂďЉBɁA̋ߎɂƂÂiqۓvZ@̊JƁA\t-|A\ɂV~[VOWۓ_̍vZƏڍׂɔrʂ񍐂B { IC

### _wRLEifqj

 2021N928i΁j16F3018F00 j @ iwj uwv ̍uł́AC^[lbg̃\[X(On-Line Encyclopedia of Integer Sequences (OEIS) [1]Inverse Symbolic Calculator (ISC) [2]ȂǁjgāǍnɂ錵Ȍʂ𔭌@ЉBȗOł́AlvZɊÂguesswork"Â悤ȌʂꂽÓTIȗЉB̌A㔼ł͍uҎgʎq̌ñf𒲂ׂőՓIȑ̌Љ [3,4]BԂ΁Ĉ悤ȃAv[Ŏ舵ȁAɂĂЉB [1] https://oeis.org/ [2] http://wayback.cecm.sfu.ca/projects/ISC/ISCmain.html [3] E. Iyoda, H. Katsura, and T. Sagawa, Phys. Rev. D 98, 086020 (2018). [4] N. Sannomiya, H. Katsura, and Y. Nakayama, Phys. Rev. D 95, 065001 (2017). { IC

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 2021N921i΁j16F3018F00 _ K iVj u}bZW[VwŒTd͔g̋Nv LIGO/Virgo ɂd͔g̏oȍ~A{̌҂͉EߐԊO ]gďd͔gCxgǊϑ錤O[v J-GEM gDA dgΉV̂̔Ƃ̕ߒ̉𖾂ڎwĂB{Z~i[ ́AdgΉV̂߂ē肵CxgGW170817 ͂߁A3rd observing run ɂJ-GEM ̊Ač̓W]ЉB { IC

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 2021N720i΁j16F3018F00 { Ύ iswbwj uAnomaly and Superconnectionv ʂ̍WɈˑ悤ȃtF~Iɑ΂Am}[𓡐삳̕@pĉ͂Aꂪ 1980N Quillen ɂēꂽ superconnection pŏ邱ƂBāẢpƂāAʂω邱Ƃɂ interface ⎞̋EnɂAm}[c_B { IC

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 2021N713i΁j17F0018F30 R a iUniversity of Portsmouthj uF_XP[ł̏d͗_̌؁v ݃_[NGlM[̐̂TlXȉF_Iϑv悳ĂB{uł́ÅϑpAۓ_KpłXP[ɂ郂fɈˑȂd͗_̌ؕ@ɂďЉB܂AXP[ł́AÑV~[VpʑΘ_𒴂闝_̌؂ɂďЉB { IC

### _wRLEifqj

 2021N76i΁j16F0017F30 i CI i{q͌J@\VXevZȊwZ^[j uiqQCDɂ鎩ȊwKeJ@Fxۏ؂ꂽ@BwKɂV~[V̉v iq̃Q[W̗_łiqʎqF͊w(QCD)̃V~[V́AvZ@̔WƂƂɔWĂBčłAX[p[Rs[^̏dvȗpړÏłBߔNA@BwK삪傫iWĂA^]╶FAFAЉ̗lXȗ̈ɓKpȂn߂ĂBāAw̕ɂ@BwK𓹋Ƃėp錤ɍsĂBiqQCD̗Oł͂ȂAvZ@ƌvZZp̐iW͂̐̕iWĂB @BwK͉͕킷邱ƂӂłBł́An~gjA邢̓OWA@BwKŖ͕킷邱Ƃ͉\낤HAIWĩOWǍvZRXgɍꍇÃOWAj[lbg[NɂvZRXg̒ႢLOWAɒu邱Ƃł΁AV~[V͍BŁALOWA͂܂ŋߎȂ̂ŁA̋ߎ̐xɍEȂV~[V@\zKvB̓ȊwKeJ@ł[1]B́AȊwKeJ@̊{RZvgƌʂɂďqׂƂƂɁAŋ߂̐[2]łQ[Wςȃj[lbg[N̍\zɂ鎩ȊwKnCubheJ@ɂĂЉB { IC

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 2021N629i΁j16F3018F00 | r i_ˑj uSpiky strings in de Sitter spacev _̘gg݂ŃhWb^[邱Ƃ́Ả݂F⏉F̉cŏdvȉۑłB̉ۑ̉֌Ė͌^\zɍsĂA͌^̌Ȏ舵Ƃ疞̂ɂ͎ĂȂBނ낻̍̂߂ɁA_ł̓hWb^[͎łȂƂᔻIȗ\zȂĂB{uł́A_ƃhWb^[̐̌؂OɁASpiky stringƌĂ΂NX̌ÓT𒲂ׂBāASpiky string̃XyNghWb^[ɂ鍂KXsԂ̎ʉ(Higuchi bound)ƒGȂƂm߂BŌɁAꂽXyNĝƂł̍GlM[UɂĂc_B { IC

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 2021N622i΁j17F0018F30 g T iswA_ˑwj ud͕󂷂鐯̉f̐lIE͓IvZv ϑZp̐iɂāAd͕̏uԂ邩ȂɂȂĂĂ܂B̍uł́AƋ҂􉽌wߎɂČvZd͕̉fЉ܂B̌̓j[gmϑƊ֌W\A̕ł̔W̉\c_Ǝv܂B { IC

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 2021N615i΁j16F3018F00 { l iHw@wj uExact solution for wave scattering from black holesv {ułKerr-Newman-de SitterɂTeukolskyɑ΂ǏzC֐pAт𗘗pU̒莮ɂĐBpƂāAŗLUAgreybody factorAGreen֐ȂǂɐGB { IC

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 2021N68i΁j16F3018F00  iKEKj uThermalization of Yang-Mills theory in a (3+1) dimensional small lattice systemv GlM[dCIՓˎ̌ʂ́CՓ˒ƂĂ^CXP[ŌnM邱ƂĂDɎʂ́C傫ȌqjՓ˂łȂqjՓ˂ɂĂM邱ƂĂDۓ_ɊÂ͂ł́C̃^CXP[邱Ƃ͍łDX́CSU(2) Yang-Mills_̔Mɂ(3+1)̏ȊiqnpĔۓIɉ͂D̓IɂKogut-Susskindn~gjApCGaussSƂŕIȃqxgԂ\CVfBK[𐔒lIɉƂłǂ̂悤ɔMN邩ׂDX́C㌋ɃNGꍇɁCn͔M̔MtԂւ̊ɘaԂtԂ̉xTƂɁC2/TƐł邱Ƃ킩D܂CSU(2) Yang-Mills_̃XNuOɂĂc_D { IC

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 2021N61i΁j16F3018F00 R (V) uԊ߂̓oCXyNgpnKEX̌؁v Ct[V_̊ϑI؋ȂA̔҂̖O͗jɎc邱ƂɂȂł傤Bnd͔gƕсACt[V_ϑIɌ؂邽߂̍łdvȎwW͌nKEX(Primordial Non-Gaussianity: PNG)łBPNǴAʏFh炬̂R_vpđ肳܂ACMBFUEɋ߂ÂĂ邱ƂAߔNł͋̓NX^OpPNG𐧌邱ƂɊ֐SW܂Ă܂BA͂̃oCXyNg̃G[́Ad͔ɂ鍂̓vʂȂKEXG[xzIłA̓oCXyNgPNG̗L]ȃv[uƂȂ邩ǂ͕Kł͂܂B{ł́A͖xꂩxč\ƂA΁gԂ̊߂hƂ@pāA̓oCXyNg̔KEXG[}錤s܂B̓Iɂ́A4000̓ƗN-bodyV~[VpāAK͂ȋ̓TCỸ_[N}^[n[č\邱ƂŁAoCXyNg̋U𐄒肵܂B̌ʁAK͂ȃXP[ł́Ač\ꂽn[̃oCXyNg̋ÚAKEX^̗\ɋ߂ÂƂ킩܂B܂AtBbV[͂sA͂̃oCXyNgɂPNG̐\ƂAč\̃oCXyNg͍č\ÕoCXyNgɔׂPNG̐3{߂ɉPł邱Ƃ킩܂Bȏ̂ƂA̓oCXyNg̍č\́AႦΓ{哱邷݂vWFNĝ悤ȍ̋̓T[xCɂāAPNGVOi𐧌邽߂ɏdvȖʂƂƂȂƊ҂܂B { IC

### _wRLEifqj

 2021N525i΁j16F3018F00 Rc a (KEK) uN=2 is largev We study the dependence of the free energy density of the four-dimensional SU(2) Yang-Mills theory at zero and high temperatures with lattice numerical simulations. The subvolume method to create a Ɓ0 domain in the lattice configurations enables us to successfully calculate the energy density up to Ɓ3/2. At high temperatures we obtain results predicted by the instanton computations. By contrast at zero temperature we find that the theory exhibits spontaneous CP breaking at = in accordance with the large N prediction. We therefore conclude that the SU(2) Yang-Mills theory is in the large N class. The surface tension of the Ɓ0 domain turns out to be negative at T=0. { IC

### _wRLEiFj

(Date) 2018N522i΁j16F4018F10 (Tuesday, May 22, 2018, 4:40 pm - 6:10 pm) Filipe C. Mena (Univ. Minho, Portugal) uSpacetime matching: models of black hole formation and gravitational wave emissionv Since the pioneering works of Oppenheimer-Snyder and Einstein-Straus, the theory of spacetime matching has been used to build models of isolated objects in astrophysics, as well as objects embedded in cosmological models. In this talk, I will describe some applications of this theory to the modelling of black hole formation, as well as radiation emission through matching surfaces, using exact solutions of the Einstein equations. If time permits, I will also present results about perturbed (non-exact) spacetime matchings, and an application to stationary axially symmetric vacuoles embedded in cosmological models containing small perturbations, including gravitational waves. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(4232)(room 4232, 2nd floor)4412(room 4412, 4th floor)

### _wRLEiFj

 2018N515i΁j16F4018F10 iswj ud͔go̘A̓ہv ۂ͕Ȋŵ݂Ȃ炸wHwȂǂłLϑĂB{uł͏d͔go2̘Aɂč\KwI4̌n̐ic_B āÂ悤Ȍn𓯊Ԃֈނ߂̃JjYBɁAɎ鋻[VwIۂЉB { wr܃LpX4 4412

### _wRLEifqj

 2018N58i΁j16F4018F10 T T iswbwj uNew Properties of Large-c Conformal Blocks from Recursion Relationv 񎟌zOtBbNCFT𗝉邤ŁAlarge-cɂ鋤ubN̐𒲂ׂ̂͏dȈӋB{uł́A܂܂ȋ̊Oѓlarge-c ubNUhRtċApĐlIɉ͂ʕƂɂĉBAv[ƂẮAċApď珇ɏ\傫܂łvZāA̐U镑ʍ̐\zƂ̂łBɂAŐc/32𒴂ƁAubN̒萫IȐU镑傫ς邱ƂAlIyщ͓IƋɗ\zBXɁAubN̋WJWCardŷ悤ȊȌȑQߌƂ\zꂽB̗\zHHLL Virasoro blocǩʂƖȂmFłBŌɁA̋ubN̐瓱OTOCG^OgEGgs[Ƃʂ̐ɂċc_BɗNɗp̋c/32𒴂邩ۂɂāAǏNԂɑ΂郌jEG^OgEGgs[(n2)̎ԔW̐U镑ωAc/32𒴂̐U镑͂镁ՓIȌŗ^邱ƂɂĐB { wr܃LpX4 ֍u(4232)

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 2018N51i΁j16F4018F10 rc u iÉj uMaximal Luminosity Conjecturesv Maximal Luminosity ConjecturéAF̗lXȕIȌno郋~mVeB[ɂ͏݂ƂłAGibbonsɂĒ񏥂ꂽB{uł́ẢȂ҂̂AǂقǕՓIɐ鉼Ȃ̂ɂāAvlʂċc_B { wr܃LpX4 4412

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 2018N424i΁j16F4018F10 C iwj uOPE for Conformal Defects and Holographyv We study the operator product expansion(OPE) for scalar conformal defects of any codimension in CFT. The OPE for defects is decomposed into gdefect OPE blocksh, the irucible representations of the conformal group, each of which packages the contribution from a primary operator and its descendants. We use the shadow formalism to deduce an integral representation of the defect OPE blocks. They are shown to obey a set of constraint equations that can be regarded as equations of motion for a scalar field propagating on the moduli space of the defects. By employing the Radon transform between the AdS space and the moduli space, we obtain a formula of constructing an AdS scalar field from the defect OPE block for a conformal defect of any codimension in a scalar representation of the conformal group, which turns out to be the Euclidean version of the HKLL formula. We also introduce a duality between conformal defects of different codimensions and prove the equivalence between the defect OPE block for codimension-two defects and the OPE block for a pair of local operators. { wr܃LpX4 ֍u(4232)

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 2018N417i΁j18F3020F00 j iwj uHigher-order scalar-tensor theories and cosmological perturbations: Can we go beyond Horndeski?v Horndeski_Euler-LagrangeX2KƂȂ悤ȍłʓIȃXJ[e\_łA SȃXJ[e\_̍Lgg݂^BߔNHorndeski_zSȗ_ Ă̂́Ȃ͉F_Iۓ̉ŕs萫ƂmĂB{uł́A K܂񂾃XJ[e\_̌𕜏KAXĂVȏd͗_ɂ l܂̐ۓc_Ad͗_̊ǧETB [Ql: KT and Tsutomu Kobayashi, JCAP 1711, 038 (2017)] { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2018N49ij16F4018F10 (Monday, April 9, 2018, 4:40 pm - 6:10 pm) Prof. Piljin Yi (KIAS) uWitten, Cardy, and the Holonomy Saddlev This talk will explore topological invariants of susy gauge theories, with some emphasis on index-like quantities and the notion of holonomy saddles. We start with 1d refined Witten index computations where the twisted partition functions typically show rational, rather than integral, behavior. We will explain how this oddity is a blessing in disguise and propose a universal tool for extracting the truely enumerative Witten indices. In part, this finally put to the rest a two-decade-old bound state problems which had originated from the M-theory hypothesis. Along the way, we resolve an old and critical conflict between Kac+Smilga and Staudacher/Pestun, circa 1999~2002, whereby the notion of H-saddles emerges and plays a crucial role. More importantly, H-saddles prove to be universal features of supersymmetric gauge theories when the spacetime include a small circle: H-saddles are explored further for d=4, N=1 theories, with much ramifications on some recent claims on Cardy exponents of their partition functions. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(4232)(room 4232, 2nd floor)

### _wRLEifqj

 2018N130() 16:40--18:10 { Ύ iswbwj uω錋萔Ώ̃Q[W_ƃu[v 萔Aƃp[^⎿ʂȂǂ̃p[^̍WɈˑ󋵂lAΏ̐Iɕۂ邽߂̏𓱂A񎩖ȉ^B܂An̂_ɂu[\A̗_̌ʂ̈ꕔ𒴏d͗_̉͂ɂčČł邱ƂB { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 123 () 16:40 ~ 18:10 剺 ė_ ( RESCEU) ubNz[nʂ̔I\ringdownd͔gv ʎqd͗_ŗ\镪U֌W\omega^2 = k^2(PlanckTCYł)́AubNz[(BH)ringdownd͔g(BHɐۓ^ۂɕod͔g)ɉe^Ƃ̂ÃZ~i[ł̓ełBringdownd͔gBȞŗLU[h(Quasi-Normal Modes: QNM)\ĂAQNMRegge-Wheeler(d͏ł̔g)̉ɁAK؂ȋE(BHŊO̐isgABHnʋߖTœ̐isg)ۂƂœBȂABHnʕt߂ɔI\݂BȂ΁AgPlanckTCYɂȂ܂ŏd͓IΈڂ󂯂̏d͔g̕U֌WA\omega^2 = k^2炸邱ƂɂȂB̂悤ȁAU֌W̋ǏIȕω͈ʂɁA̐isg̕˂NƂmĂABHnʋߖT̓d͔gA󂪔Iȍ\𔺂ꍇɂ́A˂邱Ƃ\zB̔IԂLqʎqd͗_̌̐X́A̕U֌W(PlanckTCYł)̗lqœÂ邽߁Aringdownd͔g̊ϑʎqd͗_̐\ɂB @̃Z~i[ł́ABH̔I\yringdownd͔gɊւĎZɃ[sAI\ۂBHnʂɓ݂ĂꍇɁAringdownd͔gǂ̂悤ɕύX󂯓̂c_B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2018N119 () 13:15 ~ 14:45 FK() uX-ray bound on density of primordial black holesv Primordial black holes interacting with interstellar medium gas would emit significant fluxes of X-ray photons through Bondi-Hoyle-Lyttleton accretion. These X-ray emitting PBHs would contribute to the observed number density of compact X-ray objects in galaxies. The latest X-ray data can set a new upper limit on the abundance of PBHs in order not to overproduce the observed X-ray source density. Stellar and intermediate mass PBHs can not account for the whole dark matter density. { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N1226() 16:40--18:10  T iswbwj uHolography from scalar field theories and a realization of AdS/CFT correspondencev ̍uł́A܂At[pāAdXJ[̗_Holographyi_d+1ւ̊gj@񏥂BHolographicȗ_ɂ́AUꂽvʂƂėʎq񗝘_Burresvʂ邢HelstromvʂƌĂ΂̂邱ƂBXJ[ƂCFT(Conformal Field Theory)lƁA̗Uꂽvʂd+1AdSԂLq邱ƂB̏ꍇAd̗_̃RtH[}Ώ̐d+1ł́AAdSԂIsometryɂȂ邱Ƌc_A̓IȌvZȂĂAdSԂ邱Ƃۏ؂@\𖾂炩ɂB̕@ACFTȂԂɒꂽꍇɓKp̌ʂɂĂc_BԂ΁AHolographicԂ̃XJ[̓֐GlM[^ʃe\̌vZȂǂ̍ŋ߂̌ЉB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N1219() 16:40--18:10 n I iwj uԂɂ鎞Ԍ̔񑶍ݐv m[xܕw҂Wilczek2012NɒĂAȋc_̑ΏۂƂȂuԌvɂĐUԂBƂƊԂ╽tԂŋN蓾ƂꂽԌł邪AX̒Ăł͂uvmɂ͗^ĂȂBX͒ւƂꂩ̒^ÄӖł̎Ԍs\ł邱Ƃ̂ŁA̋c_ЉBߔNꂽOꒆɂ鎞ԌƂ̊֘AɂGB Ref: HW and Masaki Oshikawa, PRL 114, 251603 (2015) { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N1128() 16:40--18:10 iswbwj uHolographic Entanglement of Purificationv We study properties of the minimal cross section of entanglement wedge which connects two disconnected subsystems in holography. In particular we focus on various inequalities which are satisfied by this quantity. They suggest that it is a holographic counterpart of the quantity called entanglement of purification, which measures a bipartite correlation in a given mixed state. We give a heuristic argument which supports this identification based on a tensor network interpretation of holography. This implies that the entanglement of purification satisfies the strong superadditivity for holographic conformal field theories. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2017N1121 16:40-18:10 HÁ@Viw Kavli IPMUj ug炬FK͍\ɋyڂev ݊ϑF̑K͍\͌nx炬d͂ɂĔʂłB{Z~i[ł́A̒łg炬ƒZg炬Ԃ̔[hJbvOɒڂċߔN̐iWBɁAFIɓłĂAL̈ɒg炬񓙕ȍՂcƂAZg炬̊ϑ璷g炬̏o\ɂĂc_B { wr܃LpX42K4232i֍uj

### _wRLEifqj

 2017N1114() 16:40--18:10 ^ iswj uSachdev-Ye-Kitaev͌^ƃJIXv Sachdev-Ye-Kitaev (SYK)͌^2015NɒĂꂽA(0+1)N̃tF~I_4̑ݍpʎq͊wnłBN傫GlM[̋Ɍł́A֌W̌vZɌFeynman_CAǑȑグłAΏ̐Bɂ̂Ƃ񎞊ԏ֊֐(OTOC)̎Ԉˑɂ݂郊AvmtwAubNz[Ŋ҂JIX邱ƂȂǂA(1+1)AdSԂ̃ubNz[ƃzOtBbNΉƊ҂A}ɐiWĂB u҂́A (1) SYK ͌^̌iqɕ߂pqnɂ[1]A (2) SYK ͌^ɂ钷Ԃ̑֊֐̐Uƃ_s̊֘A[2]A (3) SYK ͌^ɃtF~ĨzbsOɑ2̍ĕό nł̃JIẌ萫[3] ȂǂɂČi߂ĂB{uł́ASYK ͌^̌󋵂X̌̓@ɂĐƁA܂A(1)(2) ̌̊TvqׁAŁA(3) ɂďڂЉBԂ̗]T΁AɊ֘AĒׂĂAȇ厩RxÓTJIXñAvmtw̕z̋ʐ [4] ɂĂGꂽB [1] I. Danshita, M. Hanada and M. Tezuka, gCreating and probing the Sachdev-Ye-Kitaev model with ultracold gases: Towards experimental studies of quantum gravityh PTEP 2017, 083I01 (2017) [arXiv:1606.02454]. [2] J. S. Cotler, G. Gur-Ari, M. Hanada, J. Polchinski, P. Saad, S. H. Shenker, D. Stanford, A. Streicher and M. Tezuka, gBlack Holes and Random Matricesh JHEP 1705, 118 (2017) [arXiv:1611.04650]. [3] A. M. Garcia-Garcia, B. Loureiro, A. Romero-Bermudez and M. Tezuka, gStability of chaos in a generalised Sachdev-Ye-Kitaev modelh [arXiv:1707.02197]. [4] M. Hanada, H. Shimada and M. Tezuka, gUniversality in Chaos: Lyapunov Spectrum and Random Matrix Theoryh [arXiv:1702.06935]. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2017N119 16:40-18:10 ΋ _iߋEj uBMSΏ̐Əd̓[v d̓[͏d͔g̔UIȌʂłARqnd͔go[Xgʉ߂ɎRq̑Έʒûꂪɖ߂炸܂łcƂAIɊϑ\ȌۂłBߔNÃ[ʂƎ̑QߑΏ̐Aѓd͎q3̊֌W炩ɂȂĂ܂B{Z~i[ł́Ad͔g[ʂƎBMSΏ̐ǂ̂悤ɌтĂ̂A4ƍ̏ꍇr܂B { wr܃LpX43K4340

### _wRLEiFj

 2017N1031 16:40-18:10 c@iswV̊jj u Theoretical Consistency of Stochastic Approachv {uł́AhWb^[wiɂČyXJ[̒g[h̏]L^(EOM)𓱏o@ЉA̗LEOMWoƂȂ邱ƂBȂA{@͒Zg[hƒg[hԂ̔ݍp܂߂ꍇɂKp\ȏ߂Ă̎@łB܂ALEOMÓTImߒƂ݂Ȃ邩ۂɂĂc_B { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N1024() 16:40--18:10 [ icwj uIIB^_yF-_ɊÂWCŒv IIB^_yт̋ɌƂĒmF-_̗L_ɂ̓RpNgʂāÃWCꂪSL_Ɍ.{uł́AIIB^_ɂtbNXRpNgɂďЉAȉ~t@Cu[V\JrEEl̏ɃRpNgꂽF-_ɂătbNXRpNgc_.F-_ɂÂtbNXRpNgł́Aopen mirror symmetry̎@p邱ƂŁAIIB^_D-branesɕtJWČŒ肪\ɂȂ邱ƂЉ. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2017N1017 16:40-18:10 匴@RMiswj utF~IɓL̃S[XgƂ̏v tF~IɊւăOWA^2K܂ނƂłȂRAtF~Iƃ{\̑ݍp肭gݍ킹邱Ƃł̂悤ȏ󋵂ł\ĂBn~gjA͂ɂďdvł鎞ԈˑɎɒڂ邪Aϐ񕜂B { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N1010() 16:40--18:10 ː P iwȁj u1/2-BPS Wilson loop̉Zq̑֊֐: PerturbationHexagonalizationv planar N=4 ΏYang-Mills_ɂsingle-trace operatoȓ֊֐́Ahexagon form factorƌĂ΂{Iȍ\vfɕ(hexagonalization)ƂŔCӂ̌萔ŒĂꂽA̔W͉ϕ̗͂ɂƂ낪傫ϕpȂ@ɂĂ̗͖RB{ł́Ahexagonalization̊JłƂ߂ł1/2-BPS Wilson loopɑ}ꂽoperatoȓ֊֐ɒڂ邱ƂŁAWilson loopEƂđ݂邽߂ɕ̗̎ʂperturbationvZł̂ł͂ȂƊ҂A2̈قȂ錩łperturbationhexagonalization̑ΉɂČsĂB̍uł͂̌̌ɂĐB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N926() 16:40--18:10 X Y ivXgj u5d/6d DE instantons from trivalent gluing of web diagramsv g[bNJrEl̏̃g|WJ_̑S퐔z֐̓g|WJ_ƌĂ΂gݍ킹_Iʂ̑グŕ\邱ƂmĂB{ł́AVɁhtrivalent gluingh ƌĂԑ𓱓邱ƂŁAVNX̃mRpNgJrEl̂̑S퐔z֐𓾂邱ƂĂBlJrEl̂́AM_̃RpNgl̂Ȃ邱Ƃ5D^A邢E^̒Ώ̃~Y_engineer̂łBhtrivalent gluingh́AD,E^5Ώ̃~Y_non-LagrangianȌnƌSU(2)Ώ̃Q[W_dualł邱Ƃ瓱B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 Friday, July 14th, 2017, 1:15 p.m ? 2;45 p.m Hiroyuki Negishi(Osaka City University) ulFf x炬d͔g v F_̕Wfł͋Iɂ݂ƉF͈lł邱ƂƉƂč̗pĂ邪AIɌF̈l͂܂ϑIɊm߂ĂȂB̂ߔɑ傫ȃXP[̔lX̉Fɑ݂\B܂ł̔lFf̌ł͎ɋԕΈڊ֌WȂǂ̔wi̐ɂ݈̂ˑϑʂɌĂB 葽̊ϑf[^pĔlϑIɐ邽߂ɂ͔lFfł̐ۓvZKvsłB {\ł͔lFfł̐ۓ̒œɃe\[h(d͔g)ɒڂc_B Japanese Seminar Room 4232, Bldg. No.4, Ikebukuro Campus, Rikkyo University

### _wRLEifqj

 2017N718() 16:40--18:10  iwj uʎqُɋNAۂ̍ŋ߂̐iWv ߔNʎqُɋNُA(JCCʂJCQʂȂ)GlM[dCIՓˎ̕⃏CȂǂ̕ɂĊɋc_ĂDł̓JC^_Ƃ΂锼ÓT_ɊÂApċc_ĂD܂ł̌̑́Cۘ_Iȋc_łCɑΘ_IȏꍇCLorentzΏ̐Ƃ̐łD{uł͑Θ_I̗ʎq_ɊÂʎqAoCʎqُɋNAۂɂċc_D܂Cŋ߂̐iWɂĂЉD { wr܃LpX4 ֍u(4232)

### Theoretical Physics Colloquium (GR-QC Seminar)

Date 2017N711i΁j16F4018F10 Norihiro Tanahashi(Osaka Univ.) uWave propagation and shock formation in the most general scalar-tensor theory v We study the wave propagation in the Horndeski theory, one of the most general scalar-tensor theory, focusing on the shock formation phenomenon. In this theory, the propagation speeds of the scalar field wave and gravitational wave depend on the background and also their own amplitudes, and this property causes various phenomena which cannot be seen in GR. In this talk we discuss how this property affects the causality in this theory, and also study the shock formation phenomenon caused by the nonlinear effects in wave propagation. English Seminar Room 4232, Bldg. No.4, Ikebukuro Campus, Rikkyo University

### _wRLEifqj

 2017N74i΁j16F4018F10 _V iJuAgF@\j u6ꗝ_̂̐ɂāv 6ꗝ_͌݁Aɑ̗ႪĂ邪AOWAmĂ炸A̕I\ɉ𖾂ꂽƂ͌B{uł́A6ꗝ_̎̓IȐɂāAu҂̎ɂēꂽʂ𒆐SɉB܂A6ꗝ_̑\Iȍ\@𕜏KB̌A6_̃e\}ɌCX^g̐Eʗ_ɂāA̒Sdׂǂ̂悤ɌvZ邩BŌɁAe\dHiggs}Ɉڂ邱ƂŎ"small instanton transition"ƂۂɊւ邢̌ʂB { wr܃LpX4 ֍u(4232)

### Rikkyo University Theoretical Physics Colloquium (GR-QC Seminar)

Date Tuesday, June 27th, 2017, 4:40 p.m ? 6;10 p.m Maximilian Thaller (Chalmers Univ of tech.) On Static Solutions of the Einstein-Vlasov System The Einstein-Vlasov system describes the motion of an ensemble of collisionless particles in the framework of general relativity. This presentation focuses on static solutions in spherical symmetry. Three different settings will be discussed: Solutions with cosmological constant, massless solutions with matter of compact support, and solutions describing charged particles. Using properties of static solutions in the "simple setting" (i.e. no cosmological constant, no charge) and other techniques existence of solutions in the three cases is shown. Moreover, properties of massless solutions with compactly supported matter are discussed and analogies to the notion of geons are pointed out. In the case of charged particles, limits that saturate an inequality for the critical stability radius will be addressed. Some of the results are a collaboration with H. Andreasson (Chalmers Univ. of Technology) and D. Fajman (Univ. of Vienna). English Seminar Room 4232, Bldg. No.4, Ikebukuro Campus, Rikkyo University

### _wRLEifqj

 2017N620() 16:40--18:10 l iwj u[wwK: _Ɖpv @̐NAj[lbg[Nɂ@BwKٓIȃoCo𐋂Ă܂B[wwKifB[v[jOjƌĂ΂鍡̃j[lbǵAvZ@̐\◘p\ȍĩf[^ƂɌ㉟ĔWĂ܂A̖{͕Kɂ͂܂Bۂɂ͗_Il@ɊÂAASY̐̐VACfAA[wwK̐\ɂĂ܂B @̃Z~i[̑Oł͐[wwǨƏЉAj[lbg̊bƋ@BwK̃RZvgAĐ[wwKŗL̗_IACfA܂B㔼ł́A̊ȒPȎʂȂA[wwK̂܂܂Ȋg≞pЉ܂B܂Ԃ΁A[wwK̗_I𓾂悤Ƃ̐NlXɎ݂Ă錤Љ܂B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2017N613i΁j16:40-18:10 xc (kw) uGravitational Memory Charges of Supertranslation and Superrotation on Rindler Horizonsv In a Rindler-type coordinate system spanned in a region outside of a black hole horizon, we have nonvanishing classical holographic charges as soft hairs on the horizon for stationary black holes. Taking a large black hole mass limit, the spacetimes with the charges are described by asymptotic Rindler metrics. We construct a general theory of gravitational holographic charges for a (1+3)-dimensional linearized gravity field in the Minkowski background with Rindler horizons. Although matter crossing a Rindler horizon causes horizon deformation and a time-dependent coordinate shift, that is, gravitational memory, the supertranslation and superrotation charges on the horizon can be defined during and after its passage through the horizon. It is generally proven that holographic states on the horizon cannot store any information about absorbed perturbative gravitational waves. However, matter crossing the horizon really excites holographic states. By using gravitational memory operators, which consist of the holographic charge operators, we suggest a resolution of the no-cloning paradox of quantum information between matter falling into the horizon and holographic charges on the horizon from the viewpoint of the contextuality of quantum measurement. { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2017N66() 16F4018F10 Si iww@ȁj ȕ̗_̊SȒ莮 ̗̏_莮ŁARamond sector ܂ޕ̃[cςȍp\łȂƂ肪ő̏Q̂ЂƂƂĖ30NԂɂ킽ė͂ĂAŋ Neveu-Schwarz sector Ramond sector 𗼕܂ފJ̗̏_̃Q[Wsςȍp̍\ɐB͌ÓTIɊSȒ̗̏_̒莮̍ŏ̗łB܂ASen ͗]vȎR𓱓邱Ƃŕ̗̏_̃[cςȍp\@𔭓WĂB̍uł͂̒莮̌B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2017N530() 16F4018F10 c qO (sw) uGravitational wave production during inflationv It is well known that the amplitude of the gravitational wave (GW) produced during inflation is proportional to the energy scale of inflation. However, it is true only if (i) GW is described by Einstein?theory (GR)?and (ii) the GWs from vacuum fluctuation is dominant. I will discuss the cases where?the?above two conditions are not satisfied. In particular,?I will explain the new?model in which the?axion-SU(2) coupled system generates GW during inflation and its observational consequence.? { wr܃LpX42K4232i֍uj

## 2017Nxtw

### _wRLEifqj

 2017N523() 16F4018F10 iّwj uAWXE_OX_̒wv AWXE_OX_͈A̋4N=2ꗝ_ŁA㌋ɌȂ߂̕ʂvZ邱Ƃ͔ɓB{uł͉XlĂAAWXE_OX_̒w̃V[AɌ^ЉBX̌AGTΉ̒włACfA𓾂̂ŁA܂ߔNXeɂĔꂽ2JC㐔ƂłB { wr܃LpX42K4232i֍uj

### _wRLEiFj

 2017N516() 16F4018F10 c ֋v (HƑw) uF}CNgwi˃XyNgc݂̔񓙕v {ł́AF}CNgwi˂̃GlM[XyNg̎ԔWAThomsonUɌ2̉F_Iۓ_̘gg݂ňAXyNgyc݂炬Ɖx炬ō\ł邱Ƃ𓱂A@Cӂ̎̐ۓ_Ɋgł邱ƂB { wr܃LpX42K4232i֍uj

### _wRLEifqj

 2017N59() 16F4018F10 er iÉwj ut[BVv t[i܂̓n~gjASj̓CAm}[̃zOtBbNȌvZŒSIʂBd͑ɃQ[W𓱓邱ƂŉX̓t[ɃxNgwigݍ񂾁B̌ʁAxNgx[^֐ƌĂ΂ʂ𓾁A̗ʂƊ҂Ă̐ۂɖĂ邱ƂmFBƂ낪AʓIȗ_l悤Ƃƃt[̓o͔ώGɂȂĂ܂̂ŁAȒPŌnIȃt[̕ʓo^邱Ƃ͗Lvł낤Bo^EBRBXL[iBVjŒSIʂʂƃt[̗ގǋ邱Ƃł̂悤ȕʓo𓾂BBVčl邱Ƃł̓oAƑލS̖ʔގɌyASnOWAňƂ\ɂĂ邩ȂĂB { wr܃LpX42K4232i֍uj

### _wRLEiFj

 2017N425() 16F4018F10 \ iÉwj uGauss-Bonnetd͗_̈ʍ\́v F_ň闝_ʎqd͗_̕␳l_ɂ́AȗƔݍp̂B̂悤ȗ_ł́AȂŌ𒴂ꍇBGauss-Bonnetd͗_͏L̗_̈ƍlłVvȗ_łBGauss-Bonnet_̈ʍ\𒲂ׁAL̂悤ȗ_̈ʍ\c_B { wr܃LpX42K4232i֍uj

### _wRLEifqj

 2017N418() 16F4018F10 Dc ׏ iswbwj uBreaking of higher spin gauge symmetry from dual large N CFTsv Xs̃Q[W_͒_LqłƊ҂Ă邪Â߂ɂ̓Q[WΏ̐jKvB܂A3ՊEO(N)͌^ɑo΂4̍Xs̃Q[W_ɂΏ̐̔jɂĒׂB̓Iɂ́Aۓ_𗘗p3ՊEO(N)͌^ɂ鍂Xs̃Jgُ̈펟ČB̏ŁAۓ_ɂvZo΂ȗ_̌tɖ|󂵁AQ[Wꂪʂ悤ɂȂdg݂ʓIɗBɁẢ͂o΂ȍXs̗_ʂ̗_ɊgA_Ƃ̊֌WɂĂc_B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 411()@16F4018F10 ؉rY iwj uEnergy extraction from Kerr black holes by rigidly rotating stringsv ]ubNz[̉]GlM[@\, y[Y@\ȗlXȂ̂mĂ. {uł, ubNz[Ɋt̉]XgOl, ɂGlM[̕Kv⎥ɂ@\Ƃ̊֘AȂǂ̏ڍׂc_. { wr܃LpX4 ֍u(4232)

## 2016NxHw

### _wՎRLEiFj

 2017N313ij11:0012:30 Dr. Ujjal Debnath (IIEST) uAccretion of Dark Energy onto Black Hole and Wormholev We assume the most general static spherically symmetric black hole metric. The relativistic accretion of any general kind of fluid flow around the black hole has been investigated. The accretion of different types of dark energy around black hole has been analyzed and then we have obtained the critical point, the fluidfs four-velocity, and the velocity of sound during the accretion process. We have also studied the accretion of dark energy onto a Morris?Thorne wormhole. Next we have assumed some kinds of prametrizations of well-known dark-energy models. These models generate both quintessence and phantom scenarios i.e., phantom crossing. The masses of wormhole and black hole during accretion process have been obtained. The nature of mass in the late stage of the universe has been found. Also the nature of the dynamical mass of the black hole during accretion of the fluid flow, taking into consideration Hawking radiation from the black hole, i.e., evaporation of the black hole, has been analyzed. p wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2017N124i΁j16:4018:10 c V iÉwj uCMB̍t˂̂䂪ݑɂ鏉F̌؁v 1990NCOBE/FIRAS̊ϑɂAF}CNgwi(CMB)̃XyNg͍t˂ɂقڈvĂ邱ƂmĂBȂAF̐iɂẮACMB̃XyNgɍ̕˂̂䂪݂𐶂ݏolXȕߒ݂Bł̍uł́Â䂪݂̑肪lXȏF̌؂̏ƂȂ邱ƂAŋ߂̎̌ʂ܂߂ďЉB { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2017N117i΁j16:4018:10 V iswj uʑΘ_ł̘AubNz[v AtJbNz[̂̏d͔gJ,AJ̏d͔goɂČoꂽƂ͋LɐV. ̃Z~i[āJ,L̏d͔gɂĉ͓IɎ舵ƂJ\,CXnKCiKENJ^JEiKɂčl@,ʑΘ_̌؁ECɂċc_. { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N110i΁j16:4018:10 Dr. Kallol Sen iKavli IPMUj uA mellin space approach to the conformal bootstrapv We describe in more detail our approach to the conformal bootstrap which uses the Mellin representation of CFTd four point functions and expands them in terms of crossing symmetric combinations of AdSd+1 Witten exchange functions. We consider arbitrary external scalar operators and set up the conditions for consistency with the operator product expansion. Namely, we demand cancellation of spurious powers (of the cross ratios, in position space) which translate into spurious poles in Mellin space. We discuss two contexts in which we can immediately apply this method by imposing the simplest set of constraint equations. The first is the epsilon expansion. We mostly focus on the Wilson-Fisher fixed point as studied in an epsilon expansion about d=4. We reproduce Feynman diagram results for operator dimensions to O(?3) rather straightforwardly. This approach also yields new analytic predictions for OPE coefficients to the same order which fit nicely with recent numerical estimates for the Ising model (at ?=1). We will also mention some leading order results for scalar theories near three and six dimensions. The second context is a large spin expansion, in any dimension, where we are able to reproduce and go a bit beyond some of the results recently obtained using the (double) light cone expansion. We also have a preliminary discussion about numerical implementation of the above bootstrap scheme in the absence of a small parameter. p wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N1219ij16:4018:10 C r i_ˑwj uUnitarity Constraints on the EFT of Inflationv j^[ʗȂǗ_̖GlM[L_𐧌̂ɗLpł邱ƂmĂB{uł́Â悤ȗ_ICt[V͌^֘AFϑʂɗ^鎦c_Bw藝̃AiW[Ōnh炬̑֊֐ɑ΂鐳l𓱂ACt[VLqLꗝ_ɓKpBɁÂ悤Ȗ猴nh炬 subluminality KEXւ̐Vȗ_I]ƂB܂ẢFϑ𓥂܂ϑIW]ɂĂc_B { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N126i΁j16:4018:10 R i_ސwj uRecent developments in open inflationv ʎqIJڂ܂ރCt[VfI[vCt[VƌĂԁB ܂ł̊ϑɂāAX̉F̉ߋɗʎqIJڂNՂ͌ĂȂA_Iɂ݂͂̑҂ĂB {uł͗ʎqIJڂ܂މF̔WɂĊTςÅϑIȃVOiɂċc_B { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N1129i΁j16:4018:10 㓡 Đl iwȁj uoN̋ǏNԂʂČAdS̈ʍ\v AdS/CFT̋@\悭邽߂ɂƂdvȖ̈ƂAdS̋ǏCFTǂ̂悤ɌAǂ̂悤ɋLq̂ƂƂB̂ƂɃAv[钼ړIȕ@́AoN̋ǏZqɃzOtBbNɑΉCFT̉Zq邱ƂłB̃Z~i[ł͎ɂRpure AdSɂ镨ɘbBPure AdSǏZqŗNԂ́ACFTł͑ǓIϊɊւ΋ԂɑΉĂ邱ƂoBX̗͂NԂ̎ԕωprobe邽߁ACFTprimaryZqQ}֊֐̐U镑𒲂ׂBd͑o΂CFTƂłȂCFTł́Ȃ֊֐̐U镑͑傫قȂBd͑o΂悤CFT̏ꍇAǏN̎ԔW͏d͑̈ʍ\𔽉fU镑邱ƂoBԂ΂̌̌̐iWɂGꂽƎvB { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N1122i΁j16:4018:10 | W iQnwj uKerr-NewmañXJ[BSWʁv AuXgNgFߔNA]tJbNz[ɕ̗q˂邱 ɂāAۂ̒nʏāJ̗qm̏Փ˃GlLJ[C ɑ傫āJ\JwEꂽB{uāJ́ABSWʂƌ ́J邱̌ۂ̗̏_IΉɊւ錤ЉBX J[̌̕ɂĊTςA̗_I 炭BSWʂɑ΂␳ɂċc_B { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N1115i΁j17:1018:40 ^ iwj uAdS/CFTΉp񕽍tԂ̉́v AdS/CFTΉƂ́A̗ʎqQ[W_ƍ̒d͗_̑Ή֌WłB{ł͂AdS/CFTΉ񕽍tԂ̉͂ɉpB񕽍tԂƂ͋Iɂ͎ԕωȂ񕽍tԂłBႦΔMɐڂd̗铱̂Ȃǂ̈łB̂悤ȓ̂ł͔M邽ߕtԂł͂ȂA̓ł̔MƔMւ̔M̎U킪oXĂꍇ͒ԂB{ł́AAdS/CFTΉ̓Kp\ȒΏ̃Q[W_ɂāAۑdׂɊOdA̕ۑdׂ́udvn\邱ƂŔ񕽍tԂ̃fݒ肷B̌n̏d͑̋Lqł́AubNz[󒆂D-braneɔ񕽍tԂ邪AD-braneɂ͎̃ubNz[ƕʂ̋^ubNz[A񕽍tԂÂ邱Ƃ킩BɗLdזx̌nɊOdꍇD-braneKerrubNz[ɗގ̍\邱ƂA̋^ubNz[̃zCY̑xƕۑdׂ̕ϑx̊֌Wɂċc_B܂Odɂΐꂽדdqx̊ҒľvZɂĂ񍐂s\łB { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N118i΁j16:4018:10 u iwj uField-theoretic simulations of cosmic stringsv FR͂āAK͍\̑fƂȂh炬 ̂ƂČɍsĂ܂A COBE q͂߂ƂlXȍx̉Fϑɂ ے肳邱ƂƂȂǍ҂̋̒S͊OĂ܂܂B AFR͓ꗝ_⃉hXP[vIȕł͕sȐ^̑] ɕtĐẢ݂X͂GlM[XP[yɒ ۂLq関m̗_ւ̎肪ƂȂ\܂B ܂ߔNł́A_Ƃ̊֘AAF_IANVI̐Ɗ֘AāA dvȌΏۂƂčlĂ܂B {uł́A^̑]ڂRs[^ōČ iÓTj̗_IV~[VpĎۂɉFR𐶐A ̃lbg[N\̎ԐiAщFRm̑ݍpɊ֘A Љ܂B ɁAF_Iwid͔gƂẲFRɐGA JAFRlbg[Nod͔g vZ鐔lvZR[h̎^p̌ʂЉ܂B { wr܃LpX42K ֍u(4232)

### _wՎRLEiFj

 2016N111i΁j16:4018:10 Dr. Jorge RochaiUniversity of Barcelonaj uDynamics of thin-shell matter in confined spacetimes, critical behavior and chaosv I will present a study of gravitational collapse in confined spaces employing the simplest two-body setting: a system composed of two thin shells in spherical symmetry. This confined double-shell model exhibits critical behavior and chaotic dynamics, both of which are reminiscent of the turbulent instability of anti-de Sitter (AdS) recently observed in the evolution of massless scalar fields. Confinement is introduced either by putting the system inside a reflecting spherical cavity or by formulating the problem in AdS spacetime. The two shells interact only through their gravitational attraction. The problem amounts to solving just two decoupled ODEs but it captures highly non-trivial dynamics: depending on initial data, one observes prompt collapse, perpetual oscillations or black hole formation on arbitrarily long timescales. Finally, I will discuss how this extremely simple shell model heuristically supports the idea that the cascade of energies to shorter length scales is the mechanism responsible for black hole formation after multiple bounces. p wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N1025i΁j16:4018:10 Dr. Itamar Yaakov (Kavli IPMU) uMonopole operators from the 4-epsilon expansionv I will briefly review the known facts about 3d quantum electrodynamics. I will then describe the computation of the conformal dimensions of monopole operators in 3d QED using the epsilon expansion from 4d, at the one loop and two loop orders. p wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N1018i΁j16:4018:10 T iwj u萔̈قȂAFfv F̃_[NGlM[FłƂƁAʂ萔Ȃ̂ŁAFɂ̒l肵Ă\B_[N}^[CtgȂǖ̕sȕ܂߁A͑SĉFn̏FƂȂĂB̖̖݂͑Ɋ֘AĂ\BF^̑]ڂɂđI΂ꂽ萔lłƉ߂ƁAlXȉFƂɕtFƂяオĂB_ɂ鑽̐^ԂAlԌƌĂ΂X݂̑܂邽߂ɕKvȉF̏lϓ_dvȎ^͂łB{Z~i[ł́Aɕ萔قȂAFfl@Ah炬̐iɂǂ̂悤ȉe邩AɖAFm̏Փˌۂɂċc_ЉB { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N104i΁j16:4018:10 R N iwj uꗝ_̎@ɂA]Qtwist defect̗_̃ÓWJv twist defect ƌĂ΂A]QdefectiǏZqjɂčl@BɍŋRychkovTanɂĊJꂽAVÓWJ̎@(4-)O(N)Ώ̐_Wilson-FisherŒ_twist defectɓKpBɂAdefect̋ǏZq̃XP[OÂ̔񎩖ȍŒ᎟܂ŋ߂B̌ʂ͒ʏFeynman}̌vZɂÓWJ̌ʂƈvB܂Adefectlarge Nł̉͂sB { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N928ij16:4018:10 { (w) uyCEu[Ehbg𒴂 v 䂪nϑ΁AC̐FɑΉuW_vłȂBJ[EZ[K͂ăyCEu[EhbgƌĂ񂾁BQ𒴂鑾znOfAɂ͊CΘf܂łĂ錻݁Aɐ݂Ă邩ǂm邽߂ɂ́ÃyCEu[Ehbgȏ̏oϑ@m邱ƂK{łBƂɍŋߔꂽvNV}P^E̎̊Θf́Ǎ̏̕dv̂łB @X́uЂƂ̒nv̎]ɑΉāÃhbǵuFvIɕω邱ƂɒڂĂBFϓp^[ǂł΁AЂƂ̒n̏ɂ嗤CA_݂̑𐄒ł͂BɁAł͗ΐFłn̐A̗t́AߐԊÖɂĕՓIɑ傫Ȕ˗ĂAÃbhGbWƌĂ΂ĂB܂AߐԊOŊϑΐA͂܂˂^ԂȂ̂B̒̐𗘗p΁AЂƂ̒n̐FωɍԂ̊AȂ݂m鎖ł̂ł͂ȂByCEu[EhbĝȃYo鎖ŁAFwւƂȂ錤̓W]ЉĂ݂B { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N920i΁j16:4018:10 c q (w) ufWo@p1TCgtF~I͌^ɂVo[uCYۂ̉́v LxAx}̗ʎqF͊wiQCDjɂ͗lXȑ]ڂA̍\͓IɌĂB{uł͏߂ɁALxAxQCD̑}т̌ۂւ̉pTςBɁAQCDۓIɉ͂鋭͂Ȏ@łiqV~[Vɂ͗LxɂĕƌĂ΂鍢邱ƂA̍𗝉wWƂăVo[uCYۂB @u㔼ł́AfWo@ȒPɏЉɁAX̍ŋ߂̌Љ[1]BL͂Ȏ@ƂāAߔNAoHϕ̕fɊÂ̎@AfWo@уtVFbcVu@͓IɌĂBX͂̎@p1TCgno[h͌^ɂVo[uCYۂ͂[1,2]B{uł͓ɕfWo@ɂĂ̌ʂЉ[1]B܂AtVFbcVu@Ƃ̔rɊÂfWo@̉Pɂċc_B [1] Complex saddle points and the sign problem in complex Langevin simulationh, Tomoya Hayata, Yoshimasa Hidaka, Yuya Tanizaki, Nucl. Phys. B 911 (2016) 94?105[arXiv:1511.02437[hep-lat]]. [2] Lefschetz-thimble analysis of the sign problem in one-site fermion modelh, Yuya Tanizaki, Yoshimasa Hidaka, Tomoya Hayata, New J. Phys. 18 (2016) 033002 [arXiv:1509.07146[hep-th]]. { wr܃LpX42K ֍u(4232)

## 2016Nxtw

### _wՎRLEiFj

 2016N830() 16:4018:10 Anjan Giri iIIT Hyderabadj uSome interesting aspects of Flavor Physicsv Despite of many attempts we have not been successful in finding any clue about the physics beyond the standard model. After a brief introduction to the subject, I will discuss the Flavour issues we have at present. Thereafter, I will discuss how current experiments may help us to solve the problems and/or guide us to the unknown. I will conclude with the an overview of my Institute. p wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N719i΁j16:4018:10 ؑiHƑwj uConstraint on ghost-free bigravity from gravitational Cherenkov radiationv I will briefly review the ghost-free bigravity model, which is a simple extension of dRGT massive gravity. Then I discuss gravitational Cherenkov radiation in a healthy branch of background solutions in the ghost-free bigravity model. In this model, because of the modification of dispersion relations, each polarization mode can possess subluminal phase velocities, and the gravitational Cherenkov radiation could be potentially emitted from a relativistic particle. I will discuss conditions for the process of the gravitational Cherenkov radiation to occur and estimate the energy emission rate for each polarization mode. I will show that the gravitational Cherenkov radiation emitted even from an ultrahigh energy cosmic ray is sufficiently suppressed for the graviton's effective mass less than 100 eV. { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N712() 16:4018:10 V N iswbwj uRCFTɂJIXƃXNuOv ߔNAubNz[̕Ɗ֘AāAʎq̌^ɂʎqJIX̌ڂ𗁂тĂB{ł́ARCFTƌĂ΂ϕȋꗝ_ɂāAJIX̎wWł4_֊֐𒲂ׁAϕȋꗝ_̏ꍇƂ͈قȂ錋ʂ𓾂BAʎq̌^ɂJIX̎wWƂėʎq̊h(XNuO)BRCFT̗łSU(N)k WZW͌^ɂāAXNuO̎wWƂċǏIɗNꂽԂ̃G^Og̎ԔW𒲂ׂB̌ʁASdׂ傫Ɍ邱ƂŁAϕȗ_łɂւ炸XNuO̒邱ƂłB̌ʂ́A4_Ԑ̓JIXIU镑Ȃ̂ɂ炸XNuO_݂̑B { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N74ij11:0012:30 czGsiswj uFirst observation of gravitational waves : Dawn of gravitational wave physics and astronomyv First observation of gravitational waves was announced by LIGO group on February of this year. 100 years later after Einstein completed General Relativity, gravitational waves are detected at last. This announcement involved several surprise. The source of the gravitational waves was a coalescence of a binary black hole which existence was not confirmed before. The masses of the two black holes are around 30 Solar mass, which were heavier than those normally observed by electromagnetic observations. Further, Fermi Gamma ray satellite has announced that they detected short Gamma Ray burst from the In this seminar, I will explain the first observation, and future prospects of gravitational wave astronomy. { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N628() 16:4018:10 R l iJuAgF@\j uꗝ_̍s񎮂Ƃ̉pv ꗝ_̕\_͒jC̍s񎮁i2ꗝ_Kac̗ގj񏥁Eؖꂽ͍̂NɂȂĂłD͂̌̈ӖƉpC֘Aɂċc_D { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N621i΁j16:4018:10 ҋώi{wj uubNz[ϑƍŋ߂̐iWv ߔNAubNz[ӂ̑Θ_ʂllXȌvZȂĂ邪ǍʂϑʂƔrɂ͒ӂKvłBPʃubNz[̍ŋ߂̊ϑʂЉƂƂɁAϑSPAAXyNgAIUƃubNz[p[^̊֌Wɂċc_B { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N67() 16:4018:10 _ K iwj uSome implications of the 750 GeV diphoton excessv N LHC ATLASCMSɂ񍐂ꂽ 750 GeV diphoton excess ɂāAȒPȃr[̌Aŋ arXiv ɓe_ (arXiv:1602.03653, 1604.07828, 1604.07941, 1604.08307) 𒆐SɂbƎv܂B { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N531() 16:4018:10 ĒJ iw^wj uDqs񗝘_̋ϓI莮v M_̋̓I莮̉\ƂėBmĂ邢BFSSs񗝘_́A~Q[Ŵ݂ł̒莮ȂĂ炸A11̃[cϐ@ɂĎł邩́A1996Nɒ񏥂ĈȗA̖ƂĎcĂB{uł͍u҂̍ŋ߂̘_ɊÂAϓI莮񎦂B { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N524i΁j16:4018:10 S a iGlM[팤@\j uHiggs vacuum metastability in primordial inflation, preheating, and reheating v Current measurements of the Higgs boson mass and top Yukawa coupling suggest that the effective Higgs potential develops an instability below the Planck scale. If the energy scale of inflation is as high as the GUT scale, inflationary quantum fluctuations of the Higgs field can easily destabilize the standard electroweak vacuum and produce a lot of AdS domains. We discuss the Higgs vacuum fluctuations during inflation, preheating, and reheating, and show that the Higgs metastability problem is severe unless the energy scale of the inflaton potential is much smaller than the GUT scale. { wr܃LpX4 4340

### _wRLEifqj

 2016N516() 16:4018:10 q SM iw iTHESj uThermodynamic entropy as a Noether invariantil[^[ۑʂƂĂ̔M͊wGgs[jv We study a classical many-particle system with an external control represented by a time-dependent extensive parameter in a Lagrangian. We show that thermodynamic entropy of the system is uniquely characterized as the Noether invariant associated with a symmetry for an infinitesimal non-uniform time translation t->t+h, where is a small parameter, h is the Planck constant, is the inverse temperature that depends on the energy and control parameter, and trajectories in the phase space are restricted to those consistent with quasi-static processes in thermodynamics. Reference: Phys.Rev.Lett. 116, 140601 (2016). { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N510i΁j16:4018:10 Rcd iswj uʑΘ_IȎO̖ɑ΂鐳OpƏd͔gv d͔g Advanced LIGO ɂďoCʑΘ_̌؂̋@^܂ĂDʑΘ_͂܂ŘAnȂǂŋĂCȎݍpl؂͌nĂċc_ĂȂDd͎O̖̓j[gd͂ɂĂ͓IȈʉȂƂĂDC͂ĂCႦ΁COW̐Op͑znɂđΉV̂ĂDX́C̉ʑΘ_Id͏ɂčČCP̃|XgEj[gߎ̂ƂőΉ镽t𓱏ôŏЉD萫Əd͔g˂ɔpɂO̐iɂĂc_D { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2016N426() 16:4018:10 E i}gwj udXP[ʎqϕ͌^ɂ錵Ȏ-֌Wv {uł́AłPȑdXP[ʎqϕ͌^iQ̎ʃXP[TC-Sh͌^jɂāA UV AIR AőLqɂۑWard Pr邱ƂɂAȎ-֌W𓱏oB̊֌ẂAۓ_ł͑ȂۓIȏ܂ށB܂AQ[W-d͑ΉɂASɑ咴Ώ̃Q[W_̋10_UUɑ΂Ả^ʔzʎł͓̉IȓWĴłBX̎@́Aʎqϕnɑ΂Vȉ͖@ƂȂĂB { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2016N419i΁j16:4018:10 ꕽ iswj uQ[W̌ʂŐJCȌnd͔gɂāv F̃Ct[VɃQ[WꂪANVIƋĂƁApeBΏ̐jd͔g𐶐邱ƂmĂBɁAQ[W̏ꍇ͏d͔gxŐ邱Ƃł̂ŋ[B{ł́A̗lȃJCȌnd͔g̐@\ɂĐAϑ\ɂċc_B { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2016N412()16:4018:10 iswbwj u4 N=3 ꗝ_2JC㐔v {uł4 N=3 ꗝ_̂AWCԏ single vector multiplet ɗ悤Ȃ́iȂ킿 rank-one ̂́jɂċc_AɂɁiarXiv:1312.5344 ̈ӖŁjt2JC㐔𓯒肷B̃JC㐔́AN=2 super Virasoro 㐔 chiral primary anti-chiral primary ̃yAŊg債 W 㐔łAΉ4 N=3 ꗝ_ OPE ̓ BPS ZN^[LqĂB{u͗T񎁂Ƃ̋ arXiv:1602.01503 ɊÂB { wr܃LpX4 ֍u(4232)

## 2015NxHw

### _wRLEifqj

 2016N121i؁j16F4018F10 X TI iwj uNXS_kɂ{[ebNXƂẴT[tFXZqv X̓NXS_kƌĂ΂4N=1Ώ̋ꗝ_ɂăT[tFXZq𒲂ׂB܂ɊҒl^UṼNXS_k_IRɃt[ɓNX̃T[tFXZqɒڂB2N=(0,2)_̑ȉ~w𒼐ڌvZANXS_k_IRł̒wƔr邱Ƃł̃NX̃T[tFXZq𓯒肷邱Ƃ݂B2{[ebNX_̃^CvIIAu[\瓾̂łBT[tFXZqo̕@ƂāAT[tFXZqZqƂĒwɍp邱Ƃm߂B̍Zq\Ɨ\z㐔ɂĂc_B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2016N119i΁j16F4018F10 Namba Ryo iIPMU, Tokyo Universityj uPrimordial magnetogenesis with post-inflationary evolutiov There has recently been a growing evidence in the blazar observations for the existence of magnetic fields in the extra-galactic regions, where astrophysical processes are hardly responsible for their generation. One natural speculation is to attribute the production of large-scale magnetic fields to inflationary dynamics; however, such attempts have been found extremely challenging due to the strong coupling problem and severe constraints from the CMB observations. A crucial ingredient to evade such problems is a nontrivial post-inflationary evolution of the produced magnetic fields. For a significant production, the conformal invariance of a free electromagnetic (EM) field must be violated. In the case where the EM field couples to a pseudo-scalar field, the lowest-order interaction allowed by symmetries dynamically breaks parity and induces continuous production of helical EM fields. When the pseudo-scalar is the inflaton, they go through several non-trivial processes of further enhancement. On the other hand, in the case of coupling to a scalar field through the EM kinetic term, the time dependence of the coupling function breaks the conformal invariance and enhances the EM field. Since the magnetic field amplitude is strongly limited by the observations if the scalar field is the inflaton, we consider an additional field, supporting the EM production for a fixed duration during and after inflation. This scenario opens up, for the first time, a parameter window for large-scale magnetic fields that can account for blazar observation while simultaneously evading the strong coupling problem and the CMB constraints p wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4232, 2nd floor)

### _wRLEifqj

 2016N112i΁j16F4018F10 T iw@wj uCoulomb Branch Localization in Quiver Quantum Mechanicsv X́AN=4 U(1) ~ U(N)Ώ̃NCo[ʎq͊wrefined indexN[ŋǏ邱Ƃɂ茵ɕ]BN[ɂŒ_̓qbOXƈقȂ邪Aʂ͂܂łɒmĂqbOXɂǏɂ̂ƈvBN[ɂǏɂArefined index̓N[̌Œ_̃ZbgɂĂ̘aƂēB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2015N1215i΁j16F4018F10 n l iswbwj u2ꗝ_ɂdǏZqɂNԂɂĂ̗ʎqƃXNuԁv ʎqnNɂ藐Ǎn̗ʎq̓IȐUc_悤ƂƂAʎqꂪ\̂͂Ɩ₤͎̂RȂƂł낤Bnɏ\ꂪACӂ̕nő̃G^OgEGgs[𓾂ƂAn̔ȏ̎RxɂĒmȂȀԂɂĂ̏𕜌邱ƂłȂ悤ȏԂɂȂB̂ƂAnXNuꂽ(Scrambled)ƂANォ炻܂łɂ鎞ԂXNuO(Scrambling time)ƂB @X́A傫ȒSdׂ2ꗝ_ɂ Thermo-field doubleԂdZqɂNAݏʂ̎ԓIȐUXNuOԂ߂B̃XNuOԂ́ASekino-Susskind ɂ\zꂽn̎Rx̑ΐɔႷ鑬XNuO(Fast Scrambling)ԂɂȂĂAŋ߂Shenker-Stanford ɂzOtBbNȋߎvZꗝ_ōČB܂ABTZubNz[ɎR闱q̃obNANV܂߂ɂăzOtBbNȌvZsAꗝ_̌ʂShenker-Stanford̋ߎIȌʂƈv錋ʂ𓾂BX̌ʂ͋ꗝ_ɂđXNuOԂ𑊌ݏʂ炠ɌvZŏ̗łB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2015N128i΁j16F4018F10 đq a iJuAgF@\j uUΏ̋ꗝ_Ƃ̃RpNgv ߔNɑ̂U N=(1,0) Ώ̋ꗝ_AނꂽB̒ŁAX uN=(2,0)_ɃqbOX\ȗ_vƌĂԃNX̗_Ƃ̃RpNgAтƃNXS_̊֌Wc_B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N121i΁j16F4018F10 Kazunori Nakayama iTokyo Universityj uReheating Stage in Non-minimal Inflation Modelsv We study the reheating stage dominated by coherent oscillation of the inflaton field, paying particular attention to the case of inflaton having non-minimal coupling to gravity. We found a simple way to derive the effective equation of state of the reheating stage, and point out that gravitational particle production occurs much more efficiently than the case of Einstein gravity. We also discuss instability appearing in the reheating stage. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4232, 2nd floor)

### _wRLEiFj

 2015N1124i΁j16F4018F10 Katsuki Aoki iWaseda Universityj uCosmology and astrophysics in the bigravity theoryv The bigravity theory, which contains a massive spin-2 field as well as a massless spin-2 field, is attractive related to the discovery of dark energy and dark matter. We discuss the viability of the bigravity from aspects of cosmology and astrophysics. In the cosmology, although the early Universe suffers from the Higuchi-type ghost or the gradient instability against the linear perturbation, the instabilities can be resolved by taking into account nonlinear effects of the scalar graviton for an appropriate parameter space of coupling constants. On the other hand, a singular behavior of scalar graviton appears in a static compact object beyond a critical value of gravitational field strength in the parameter space, in which the maximum mass of the neutron star is constrained to evade the singular behavior. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4232, 2nd floor)

### _wRLEifqj

 2015N1117i΁j16F4018F10 c pF iRʎqȊwj upp-waves͌^ł̖̕()ɂ鑊ݍpRiemannʂ3Łv M_̍s͌^̕()ɂ鑊ݍp܂ł邩ǂ͏dvȖłB{ułpp-waves͌^ł̖̕ߒc_B̉ߒ͂̃glʂƑBAdS/CFTΉʂABJM_Ƃ̊֌WȒPɋc_ÃglʂLqBPSCX^g͍sTCY傫ꍇ3̃vXƓɂȂ鎖BXɕߒLq邽߂ɂ́AʏR^3ł͂ȂARiemannʂ̗l2R^3\荇Ԃ̏ł̉KvȂƂBۂ̃vX̉gĎۂɖ􂷂p𑨂̃vbgBStefano Kovacs(Dublin IAS), Yuki Sato(Chulalongkorn Univ., Bangkok)Ƃ̋arxiv:1508.03367ɊÂB { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N1113ij13F1514:45 Naoki Tsukamoto iRikkyo Universityj uA method to find wormholes with positive masses: Microlensing effectsv General relativity admits the nontrivial topology of spacetimes like wormhole spacetimes as non-vacuum solutions of the Einstein equations. Can we distinguish a wormhole with a positive mass from other massive objects by gravitational lensing effects? In this talk, I will review wormholes and their gravitational lenses and then I will suggest a new method to find wormholes which have a positive mass with gravitatinal lensing effects. Let us discuss microlensing effects by the light rays coming from the another region through a wormhole throat. p(English) 4341, 3rd floor, the building No.4

### _wRLEiFj

 2015N1110i΁j16F4018F10 c @C(Sousuke Noda) iÉw(Nagoya Univ.)j uWave optics in black hole spacetimes and the black hole shadowv Gravitational lensing has been discussed by some researches as a tool to investigate galaxies and massive objects such as black hole candidates. In the ordinary theory of gravitational lensing, what we consider is the motion of light ray (geometrical optics). But taking account of observations by electro wave or gravitational wave in the future, we may need to deal with the lensing problems in terms of wave optics. As an example of wave optical lensing, we discuss wave optics in black hole spacetimes. In this talk, we start with a brief review of geometrical optics in black hole spacetimes and then we will describe wave scattering problem by a black hole (wave optics). Finally as an application, we will see how to get wave optical images of black hole shadows. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4232, 2nd floor)

### _wRLEiFj

 2015N1029i؁j16F4018F10 Tetsuya Shiromizu iNagoya Universityj uRigidity and stabilityv Positive mass theorem(PMT) tells us spacetime rigidity and stability in general relativity. In this seminar, I would like to review some applications of PMT, the uniqueness of static black holes and Riemannian Penrose inequality. In addition, I will discuss PMT as a guiding principle "sense and sensibility" in model building for dark energy/modified gravity. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4340, 3rd floor)

### _wRLEifqj

 2015N1013i΁j16F4018F10 v i}gwj uʉ􉽊wɊÂd͗_̍\Ɋւ錤v ʉ􉽊ẃCd͗_̃{\ɂĊ􉽊wIȗ^鐔wIgg݂łB̘gg݂ł́CڑƗ]ڑ̒âȂŎ̌vʂłȂCKalb-Ramond܂߂Ă̏̊􉽊wIȋLq^D_ł́C̏̓KȔzʂwiƂĂ̂Ȃ̌̉^l@邪CقȂwiꓯm̔񎩖ȓƂToΐmĂĎvʂKalb-RamondƂʂ邱ƂȂɈ邱ƂCʉ􉽊wToΐ􉽊wIɗ邤łLpłƊ҂D @܂Œd͗_ōlĂ̔zʂɁCIToΕϊ{ĂƊ̊􉽊wł͑ȂC􉽊wIȏ̔zʂoƎwEĂD̊􉽊wIgg݂g邱Ƃ͂ƂCToΐ̊􉽊wI^Ɗ҂ʉ􉽊w̘głC܂܂ɋc_͂ȂĂ邪̔􉽊wIȔzʂɂĂ͈ˑRƂė[܂ ĂƂ͂Ȃ󋵂ɂD @{uł͈ʉ􉽊wɂĐڑƗ]ڑ̖ւuʉ􉽊w̕ώv𓱓邱Ƃɂ􉽊wIȔwi̐VȊ􉽊wỈ\ɂċc_DƂɂ̈ʉ􉽊w̕ώɊÂd͗_̍\ɂĕ񍐂. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N106i΁j16F4018F10 Atsuki Masuda iOsaka City Universityj uPropagation of an optical vortex in a curved space-timev Recently, optical vortices, twisted light beams like corkscrew around axes of travel, are actively investigated in laboratories. The beams carry orbital angular momentum along their propagation axes. We study orbits of an optical vortex in a curved spacetime using the eikonal approximation. We show that the equation of motion for an optical vortex is different from the geodesic equation due to 'spin-gravity' coupling. We discuss deviation of orbits from the geodesic in a Kerr spacetime. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4232)

## 2015Nxtw

### _wRLEifqj

 2015N724ij16F4018F10 oG i썂wZj u2^CvIIA_̍s͌^ɂ钴Ώ̐̎Ijv Ώ̐LAdouble-well|eV0̍s͌^ARamond-Ramondwi2̃^CvIIA_ɂlXȎނ̊{Iȑ֊֐Č邱ƂB̎͑O҂҂̔ۓI莮^邱ƂB肵A̗_̔ۓIʂɒׂB̌ʁA萔ɊւۓWJ̑SŕۂĂp[Ώ̐́A s͌^ɂCX^gʂɂĔۓIIɔj邱ƂؖB̃CX^ǵAN=2 boundary Liouville_D-braneƓ肳Ɗ҂BɁA̗_̎RGlM[̊SȓÂAۓ̑Sɂ鑊֊֐ȂǁAŋ߂̐iWɂGBɂA̗_large order behaviorǂݎ邱ƂłB { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N714i΁j16F4018F10 Ian Vega iSISSA - International School for Adbanced Studiesj uRotating black holes in Lorentz-violating gravity theoriesv There is considerable interest in the strong-field behavior of Lorentz-violating gravity theories. One point of interest is whether or not the notion of a black hole as an absolute causal boundary persists in these theories, which can sometimes propagate signals infinitely fast. Past work on spherically-symmetric black holes reveal that absolute causal boundaries exist in spite of these infinitely-fast propagating modes. These causal boundaries have come to be known as universal horizons. In this talk, I shall discuss black holes in two popular Lorentz-violating theories, Ho\v{r}ava gravity and Einstein-aether theory, and showcase progress made in exploring their rotating black holes. For Ho\v{r}ava gravity, I shall discuss three-dimensional black holes in its infrared sector. Within this setting, we have derived the most general class of stationary, circularly symmetric, asymptotically anti-de Sitter black hole solutions. I also discuss slowly-rotating black holes in four-dimensional Einstein-aether theory, which we construct numerically. Most notably, we learn from these solutions that universal horizons may not be a generic feature of black holes in Lorentz-violating theories. p(English) wr܃LpX4(Rikkyo Univ. Ikebukuro Campus, building 4) ֍u(room 4232)

### _wRLEifqj

 2015N710ij16F4018F10 u iGlM[팤@\j uM2u[猻钴ʎq͊wv {uM2u[o钴ʎq͊wc_B܂݂܂ł̌ŒmĂ钴ʎq͊wɊւ鐫Iɘ_B (0+1)̗ʎq_A܂ʎq͊wɂĒΏ̐ƋΏ̗̐̏ʎq_ɂ͌Ȃ̕ςŌ[IȐƂ B܂ԁEN 8 ܂ł̒ʎq͊w̍\ɗLpł邱Ƃc_BM_̊{ISƍlĂ閌̂̕łM2 u[̒GlM[E̐ϗL_c_B݂̗L͂ȌƍlĂ闝_BLG _AABJM _ƌĂ΂3 Chern-Simons _łA̗_͕R11 ^镽RȊ􉽂M2u[̒GlM[͊wLqƍlĂ邱Ƃ_Bq̒ʎq͊wM2 u[Ɋւc_𓥂܂ARpNgRiemann ʂɊtM2 u[lARiemann ʂ̑傫œ肳GlM[ႢGlM[Ɍŏoʎq͊wBČʂƂČʎq͊w܂ŒԁE ͍\łȂN 8 ƂΏ̐킹ʎq͊wnł邱ƂB܂ꂽʎq͊wȂM2 u[݂̌̂Ȃ炸lXȐwւ̉p̉\킹Ă邱Ƃc_B { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2015N630i΁j16F4018F10 Xc iÉwj uubNz[̃~NȏԂɊւV\ƁAQ[Wd͑Ήւ̉pv g[N̑Ołp-soup\ƂubNz[ ~NȏԂɊւbЉ܂B㔼ł́AQ[Wd͑Ή ̗\p邱ƂŁALxɂ钴Ώ̐Q[W_ŃubNz[IȐU镑@\𗝉ł邱Ƃc_܂B ABJM6d SCFTɂN^3/2 N^3 ɔႷGgs[RɃQ[W_̉͂ɂĐł邱Ƃ܂B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N623i΁j16F4018F10 N iÉwj uSpherical Domain Wall Collapse in a Dust Universev To clarify observational consequence of bubble nucleations in inflationary era, we analyse dynamics of a spherical domain wall in an expanding universe. We consider a spherical shell of the domain wall with tension \sigma collapsing in a spherically-symmetric dust universe, which is initially separated into the open Friedmann-Lema\^itre-Robertson-Walker universe inside the shell and the Einstein-de Sitter universe outside. The domain wall shell collapses due to the tension, and sweeps the dust fluid. The universe after the collapse becomes inhomogeneous and is described by the Lema\^ itre-Tolman-Bondi model. We construct solutions describing this inhomogeneous universe by solving dynamical equations obtained from Israel's junction conditions applied to this system. We find that a black hole forms after the domain wall collapse for any initial condition, and that the black hole mass at the moment of its formation is universally given by M_{\rm BH}\simeq 17 \sigma/H_{\rm hc}, where H_{\rm hc} is the Hubble parameter at the time when the shell radius becomes equal to the Hubble radius. We also find that the dust fluid is distributed as \rho\propto R^{3/2} near the central region after the collapse, where R is the area radius. These features would provide observable signatures of a spherical domain wall generated in the early universe. p wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N616i΁j16F4018F10 v _Y iswbwj uExploring tidal effects of coalescing binary neutron stars in numerical relativityv Coalescences of binary composed of two neutron stars---binary neutron stars---are one of the most promising gravitational-wave sources for ground-based laser-interferometric detectors such as Advanced LIGO (United States) and KAGRA (Japan). Advanced LIGO will begin operations from this year, and KAGRA will join the observation in this decade. Once the detection becomes a routine, gravitational-wave astronomy will serve as an important tool to study unexplored physics such as properties of neutron stars and supranuclear-density material. In particular, tidal deformability (strongly related to the radius) governs tidal deformation of neutron stars in a binary, which changes orbital dynamics and gravitational waves from those of binary black holes. To extract neutron-star properties from gravitational waves, it is necessary to prepare accurate theoretical waveforms (usually called templates) from binary neutron star coalescences. However, it is a hard task to derive accurate waveforms for the entire coalescence process, because the merger involves rapid variation of spacetimes sourced by strongly-gravitating hydrodynamical objects. Here, numerical relativity (i.e., fully general relativistic simulations) is the most reliable way to study the late inspiral and merger phases, where tidal interaction plays a substantial role. In this talk, I will summarize the current status of template preparations and present recent results obtained by our numerical-relativity simulations. p wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2015N69i΁j16F4018F10 ic jY iGlM[팤@\j uQCDLee-Yang[_zRoberge-Weiss]ځv Lee-Yang[_藝͔M͊wp[^𕡑fgۂɌ啪z֐̃[_𑊓]ڂƊ֌Wt藝łB[_藝LeeYangɂ莮̌ɁAIsing͌^։pAIsing͌^̑]ڂ݂̂Ƃ̏ؖɗpꂽB̌AAϐixjɑ΂ [__ՊE_ł̃[_̃XP[OȂǂ̗_IgsꂽB ŁA ۂ̃[_̓o͈ʓIɂ͓ۑƂĒmB {uł́AʎqF͊wɂLee-Yang[_藝̉pɂĐBiqQCDɂLee-Yang[_̌vZ@AɂLee-Yang[_͓̉IȂsBQCDLee-Yang[_e[^֐̃[_ƈv邱ƂAiqQCĎvZpĂ̌؂sB܂AߔNsĂ鑊Θ_IdCIՓˎƂ̊֘AȂǂɂĂB { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N62i΁j16F4018F10 c iwK@wj uSpin structure of black hole space-timev It is a necessary condition for a space-time to be physically reasonable that it admits a spin structure, a topological condition for the tangent bundle such that the Dirac spinor field can be defined globally. This usually does not matter when the space-time dimensionality is four, since every globally hyperbolic orientable space-time is spin, i.e. admits a spin structure. Here, we consider a higher dimensional space-time with black holes, and give a criterion whether it is spin or not. We also show that when a 5-dimensional black space-time is not spin, there appears a certain kind of black hole that is homeomorphic with a lens space. p wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N526i΁j16F4018F10 ɓ m iwRESCEUj uA novel method to determine masses of isolated neutron stars using Einstein telescopev We investigate a possibility of estimating mass of an isolated rapidly rotating neutron star (NS) from a continuous gravitational wave (GW) signal emitted by the NS. When the GW passes through the gravitational potential of the NS, the GW takes a slightly longer time to travel to an observer than it does in the absence of the NS. Such a time dilation effect holds also for photons and is often referred to as the gravitational time delay (or the Shapiro time delay). Correspondingly, the phase of the GW from the NS shifts due to the Coulomb type gravitational potential of the NS, and the resulting logarithmic phase shift depends on the mass, the spin frequency of the NS, and the distance to the NS. We show that the NS mass can, in principle, be obtained by making use of the phase shift difference between two modes of the continuous GW such as once and twice spin frequency modes induced by a freely precessing NS or a NS containing a pinned superfluid core. We estimate the measurement accuracy of the NS mass using Monte Carlo simulations and find that the mass of the NS with its ellipticity 10^{-6} at 1 kpc is typically measurable with an accuracy 20% using Einstein Telescope. p wr܃LpX43K 4340

### _wRLEifqj

 2015N512i΁j16F4018F10 dX iswbwj u􉽊wIIԃvO-ߋA݁Av ubNz[͂̃zCYʐςɔႷG gs[߁AwɂIԂ̓v ͊wIATu\Ă͂łB _ɂ閳ђ藝͏d͂ɂĂ͂̂悤 ȔIԂ݂͑ȂƂ ƂӖ邩 ɎvBA_ɂubNz[ ɊւẮAubNz[ƓʁEdׂ zCYɐł ȁu wIIԉv̓Iɍ\ĂB ̉ђ 闝ŔA(1) d>4̉łA(2)͗lXȏ ܂Chern-Simonsݍp܂ޒd͗_̉ A(3)͔̉񎩖ȃg|W[A ƂƂłB́AubNz[̔I ԂÓTd͗_̘gō\悤Ƃ u􉽊wIIԃvOvTςA vO̖ڕWƂ܂ł̐ʂłȂA ꂪ܂ޖ₻ɑ΂ᔻɂGB āAX [arXiv:1503.01463] ō ߍsA ɈʂȃNX̊􉽊wIIԂɂĐ B { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2015N428i΁j16F4018F10 c Y iGlM[팤@\j ularge D limit of General Relativityv The spacetime dimension D is a dimensionless parameter of General Relativity. Considering the 1/D expansion of General Relativity with the infinite limit of D, we find the gravity is dramatically simplified but its non-trivial structure still remains at the limit. This simplification occurs since the expansion parameter 1/D introduces the separation of scales in the theory naturally such as the horizon radius, r_BH, of a black hole and 1/D times of the horizon radius, r_BH/D. Using this simplification we can solve various problem of the gravity in analytic way. In this talk I will review some basic properties of the gravity at large D, and next I will give recent progress of large D gravity project. p w4 ֍u(4232)

### _wRLEifqj

 2015N421i΁j16F4018F10 iHƑwj ud͗_p5Ώ̐Q[W_̍\v 5Ώ̃Q[W_̉͂́AM5u[̐TdvłƍlĂBX͋ǏƌĂ΂錵vZɕKvȁAȂԏ5Ώ̃Q[W_̍\d͗_p邱ƂōsB̍\@pƁA25wi6̕ɂ֌WÂB{uarXiv:1404.0210ƐišɊÂB { w4 ֍u(4232)

## 2014NxHw

### _wRLEiFj

 2015N0123ij16F4018F10 c^ ikwj uubNz[WFbg̋쓮JjYv ubNz[V̂̒ɂ́A Θ_Ix̃vY}𕬏oĂ̂B {\ł́ÃvY}̋쓮@\ƂčŗL͂ł uubNz[]GlM[̓dIofv ̏ڍׂȕc_B ɁA̋@\ƃy[YߒƂ̊֌Wɂċc_B w4 3K 4340

### _wRLEifqj

 2015N0113i΁j16F4018F10 ۋg ꒨ iImperial College Londonj u4d N=1 SCFTs from M5-branesv In this talk we study the construction of a large class of 4d N=1 gauge theories, which flow to nontrivial IR fixed points, from M5-brane compactification on a Riemann surface including punctures which preserve N=1 supersymmetry. We find that various remarkable properties of this class of theories, like duality, can be understood in terms of the Riemann surface and leads to discovery of unknown dualities in N=1 theories. w4 ֍u(4232)

### _wRLEiFj

 2014N1216i΁j16F4018F10 LV iRwj uubNz[^V̂̉ev ubNz[VhEiwiEӌ̉Aej̓ ̕s~Ȏ݂ɗR邽߁A ȓV́i߃ubNz[^V́j ݂ƁAubNz[̓肳ȂB {ł́A^V̗̂ƂăOoX^[y GX[z[ɂĒׁA ̉Ae̓𖾂炩ɂB w4 ֍u(4232)

### _wRLEifqj

 2014N1209i΁j16F4018F10 gc Y iswj ud/Yang-BaxterΉɂāv ߔNAAdS5×S5 ̒_̉ϕό舵nIȎ@JꂽB ̎@ɊÂƁA ÓTYang-Baxter𖞂ÓTr-s߂΁A AdS5×S5 ̉ϕόɑΉd͉܂ (d/Yang-BaxterΉ)B Ⴆ΁A N=4ΏYang-Mills_(SYM)beta-όɑΉLunin-MaldacenaA ԏN=4 SYM_ɑo΂Maldacena-RussoȂǂ 悭mĂd͉ɑΉr-s񂪌Ă邵A ̂悭킩ȂɑΉr-s݂B {uł́A AdS/CFTΉ̉ϕόɊւŋ߂̌ʂɂāA s̃r[ȂЉB ܂AϕAdS5×T{1,1} ̕όւ̉pɂĂB w4 ֍u(4232)

### _wRLEiFj

 2014N1202i΁j16F4018F10 Y Dq iÉwj uh炬̐ԊO萫ƃCt[VF̏ԁv Ct[Vɐꂽh炬̐ԊO̔ʎq␳ɂ ۓ_j]\AߔNAĂB {uł́AԊO̔ʎq␳UA ۓ_Kp\ƂȂ邽߂̏c_B ɁA̐́A Ct[VF̏Ԃɑ΂A ^鎖B w4 ֍u(4232)

### _wRLEifqj

 2014N1125i΁j16F4018F10 c ͎ iwj uSuperconformal index on RP2×S1v We study N=2 supersymmetric gauge theories on RP2×S1 and compute the superconformal index by using the localization technique. We apply our new superconformal index to the check of the simplest 3d mirror symmetry and prove it by using a mathematical formula called the q-binomial theorem. In this talk, I would like to explain the crucial points of our work and comment on some generalizations. This talk is based on [arXiv:1408.3371]. w4 ֍u(4232)

### _wRLEifqj

 2014N1121ij16F4018F10 ђ T iwj uBlack Holes and Condensed Matter Physicsv We will discuss several recent developments where black hole physics and condensed matter physics have deep connection. w4 ֍u(4232)

### _wRLEiFj

 2014N1119ij16F4018F10 CY iÉwj u_̔Wv An overall picture of molecular cloud formation in the Galaxy is presented in this talk. Recent high-resolution magneto-hydrodynamical simulations of two-fluid dynamics with cooling/heating and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of compressional events. Indeed, multiple compressions of ISM create both massive filamentary molecular clouds whose axes are perpendicular to the magnetic field lines and faint striations that are parallel to the field lines, which mimic general features of actual observations. Subsequent collapse and fragmentation of filamentary molecular clouds provide the initial conditions of protostellar collapse calculations that have been done extensively and successfully. This finding enables us to envision a scenario of molecular cloud formation as the interacting shells or bubbles in galactic scale. We estimate the ensemble-averaged growth rate of the individual molecular cloud, and predict the mass function of molecular clouds. This picture naturally explains the accelerated star formation over many million years that was previously reported by stellar age determination in nearby star forming regions. Recent claim of cloud-cloud collision as a mechanism of forming massive stars and star clusters can be naturally incorporated in this scenario, which explains why the massive stars formed in cloud-cloud collision follows the power-law slope of the mass function of molecular cloud cores repeatedly found in low-mass star forming regions. w4 3K 4340

### _wRLEifqj

 2014N1107ij16F4018F10 C iwj uSupersymmetric Renyi Entropyv The Renyi entropy is a one-parameter generalization of entanglement entropy that can be a useful order parameter for various phase transitions. In QFTfs, it is calculated using the so-called replica trick that reduces the computation to the partition function on a singular space. This method, however, is not compatible with supersymmetry in general. In this talk, we define the supersymmetric extension of the Renyi entropy by introducing a chemical potential for the R-symmetry in N=2 supersymmetric gauge theories in three dimensions. Using the localization method, we write down the matrix model representation that allows us to examine its properties such as the duality invariance, the large-N behavior and the expansion with respect to the parameter. We also discuss the gravity dual and the higher-dimensional counterparts as well. w4 ֍u(4232)

### _wRLEiFj

 2014N1023i؁j16F4018F10 q iHƑwj u񓙕Ct[Vɂnh炬člv 񓙕Ct[Vf́A Ct[VFɂ閳щjŏ̔łA ܂ʏł͌Ȃnh炬̐\A _IɂϑIɂ[fłB {uł́Anh炬̉͂člA {f\znh炬̓vI񓙕ɂāA ܂łƂ͈قȂ闝_I\^B w4 ֍u(4232)

### _wRLEifqj

 2014N1017ij16F4018F10 O ibwj uQuantum Entanglement of Local Operatorsv ߔNAlXȕɂ(\)G^OgE Ggs[ڂW߂ĂB ŉX́AǏZqɂėNꂽԂɑ΂ ̃Ggs[̐𒲂ׂB ʁAnSԂ̔Ɏ(\)G^OgE Ggs[萔ŗ^A ̒l}ꂽZqɈˑĂ邱ƂoB ܂A̒萔pĉZq(\)G^OgE Ggs[ƂʂB ̉Zq̃Ggs[ɂĉZq̕ނo邱Ƃ҂B ̔\ɂĉX͉Zq(\)G^OgE Ggs[̎Ƃ炪]ׂaɂĘbƎvB w4 ֍u(4232)

### _wRLEiFj

 2014N1010ij16F4018F10 icwj u̒ł̏d͕v ߔNAnti-de-Sitterł̏ď͕ɂA Ԃɂg̃GlM[JXP[hۂ ubNz[ɏdvȖƎwEꂽB ͗ႦΑQߕRȎłIȕߋ@\΋N肤邩B {\ł͂̊̕ȒPȃr[ƂƂɖ𖾂̖ɂċc_B w4 ֍u(4232)

### _wRLEifqj

 2014N0930i΁j16F4018F10 ߓ c itwj uStability of chromomagnetic condensation and mass generation for confinement in SU(2) Yang-Mills theoryv NH[N߂̑oΒЂƂ͓̉IƂ SU(2) Yang-MillsɂĈlȐFCIÏkSavvidy^ 1977Nɒ񏥂ꂽB C̕s萫NielsenOlesenɂĒɎwEC Ryn[Q^XpQbeB^󂪒񏥂ꂽB C1970NȌC̕s萫菜lXȓw͂ȂĂB Nielsen-Olesens萫́CFɊւL|eVC P|[v̌vZł́CŒŗLlɌ^LI[hNāC 񎩖ȋƂɋNĂB uł́C߂ɁCNH[N߂Ɋւŋ߂̌̊ȒPȃr[sB ɁCĊ֐肱݌Q̕@pāCSavvidy^Nielsen-Olesens萫 ĂȂȂ邱ƂB ̌_́C(i) ȂLύpC fɒlLύpɑ΂t[̌Œ_ƂāC Cӂ̐ԊOؒfɑ΂Ď邱ƁC (ii) \傫ȐԊOؒfɑ΂ẮC ȂߎI͉̓Iɋ߂邱ƁC]B ɁC\ȐԊOؒfɑ΂ĂCŒ_ɂƂǂ܂C܂C 萫ێ邽߂̕I@\ƂāC ʎ2BRSTsςȐ^ÏkɂăO[I̎ʐN邱 iO[{[ƓꎋłQO[I ̑ԂƊ֘AjwEB w4 ֍u(4232)

### _wRLEiFj

 2014N0926ij16F4018F10 @^O iwj uՓ˃vY}n~~Ղł̗qƊp^ʗAv Fł̍~~Ղ͏d͉]n̕ՓIȍ\łA ߔN~~Ղێp^ʁEASJjYƂ C]šd̂̃V~[Vɂ萸͓IɂȂĂB AubNz[V̂̍~~Ղł́A dqƃCỈxقȂvY}MIȍGlM[dqϑĂA Փˌnł̍~~Ղ̕dvƂȂĂĂB Z~i[ł́AՓˌn̍~~Ղł̗̍q p^ʗAɂčŋ߂̌ЉB w43K 4340

## 2014Nxtw

### _wRLEiFj

 2014N0715i΁j16F4018F10 iHƑwj uɂ郏[z[Ƃ̓I萫v F̓̍ʑΐ_ŐÓIȃ[z[ ̈萫ɂċc_܂D massless̃XJ[iS[Xgĵ݂ŁC Ellis̍łłD 萫ɊւĂ͐ۓɑ΂̂Ɣ̌vZʂЉC Ԃ΃KEX{l̉eɂĂb܂D w4 ֍u(4232)

### _wRLEifqj

 2014N0708i΁j16F4018F10 Y s icmwj uΏ̊iqQ[W_̐^Ƃ̌Œɂāv iq̒Ώ̃Q[W_̈ƂāAʏ̊iqQ[W_ƓlA j^[ȃNϐƂăQ[W̎Rx\_ ɂč\ĂB̗_́A Q[WQƂU(N)ł͂ȂSU(N)Ƃ锽ʁA Q[W̔zʂƂĔ񕨗IȐ^󂪑݂Ă܂ Ƃ肪mĂB ]́A NϐadmissibilityۂƂ 񕨗IȐ^ւ̑Jڂ֎~ĂÂ߂ɍpGɂȂA lvZ̖WɂȂĂB X͍A Nϐ̓Hv邱ƂɂāA admissibilityۂƂȂɔ񕨗IȐ^ւ̑Jڂ֎~A IɕIȐ^݂̂悤ȗ_\邱ƂɐB ̃g[Nł́AiqQ[W_̊{IȎ Ώ̃Q[W_iqɒ@ɂĂ̈ʘ_A X@ɂĐB w4 ֍u(4232)

### _wRLEifqj

 2014N0701i΁j16F4018F10 l iwj uSeiberg Duality, 5d SCFTs and Nekrasov Partition Functionsv We propose a duality between various Type IIB 5-brane web configurations, and this conjecture implies an equality between the corresponding 5d Nekrasov partition functions (i.e. refined topological string partition functions) that are associated with local del Pezzo surfaces. It is known that M-theory compactified on a local Calabi-Yau 3-fold leads to a 5d superconformal field theory (SCFT), and this system is dual to a Type IIB 5-brane web system. One can expect that the gPicard-Lefschetz transformationh of these 3-folds implies the duality between these brane setups and the resulting 5d SCFTs. We then find that many different Type IIB 5-brane webs describe the same 5d SCFT that was found by N.Seiberg. We check this duality by comparing the Nekrasov partition functions of these 5-brane web configurations. w4 ֍u(4232)

### _wRLEiFj

 2014N0623ij12F2013F30 Remya Nair iJamia Millia Islamiaj uProbing the cosmic distance duality relationv The inferences we make from cosmological observations have some underlying assumptions. Sometimes these assumptions are so common that they are overlooked. In this talk I'll discuss the observational analysis of a consistency relation, the *distance duality* relation, which can be used to test the validity of some of the fundamental assumptions in Cosmology, and can further be used as a consistency test between different distance probes. w4 ֍u(4232)

### _wRLEiFj

 2014N0617i΁j16F4018F10 Sanjay Jhingan iJamia Millia Islamiaj uGravitational Collapse: Causal Structure of Singularity.v It will be a technical extension of first two lectures so students will be able to understand. I will use dust model and discuss global and locally naked singularities. Some new results which I derived last month. w4 ֍u(4232)

### _wRLEifqj

 2014N0613ij16F4018F10 R D iJuAgF@\j uu[gXbvŗ鑊]ڂƗՊEہv ߔNAu[gXgbv̋ꗝ_ɁilIɁj Kp鎎݂傫Ȑʂ𓾂ĂBႦ΁AߔNA R̃CWO͌^Ώ̐uꂽv Ƃ͋LɐVB{uł́A ܂ő̕@ł͗_I͂ł tXg[VXsn QCD ̃JC]ڂ̑]ڂ̎̌ƗՊEw̏ɂ u[gXgbv O(n) x O(m) ̑Ώ̐R̋ꗝ_ɗp邱Ƃɂ ۓIɋc_B ΒmM(Kavli IPMU)Ƃ̋ arXiv:1404.0489 ɊÂB w4 ֍u(4232)

### _wRLEiFj

 2014N0603i΁j16F4018F10 x^ iHȑwj u~Ώ̂Ȕd͔gv QOOTNAPomerankỷǂtU@ɂāA ubNOꂽƂ_@ɁA ̍ubNz[ĂB {ł́Ảǌ^tU@߂ĉ~Ώ̂ȎɉpA ud͔gvLqV߂B {Z~i[ł́A܂tU@̃r[A {ŋ߂ЉƂƂɁA d͔g̔ʁit@f[ʁjɂĂc_B w4 ֍u(4232)

### _wRLEifqj

 2014N0527i΁j16F4018F10 ɓ xq iGlM[팤@\j uiqV~[VgConformal windowɊւŋ߂̌ɂāv lQ[W_ɂ 񎩖ȑݍpԊOŒ_݂t[o[̗̈ conformal windowƌB ߔNAconformal window݂̑A ۓ_I@łiqV~[VpĒTA ̐ԊOŒ_ł̗̋_̐ ۓ_Iɒׂ邱Ƃł悤ɂȂB {uł́Aŋ߂̂̎ȌЉA Œ_T@񎩖ȌŒ_ɂՊEw̓o@rc_B w4 ֍u(4232)

### _wRLEiFj

 2014N0520i΁j16F4018F10 iÉwj uF_I2ۓ_Ő2d͔g̉𖾁v F_Iۓ_2ւƊg邱ƂŁA 2d͔gKRIɐB 2d͔ǵA_N邽߂ Kׂ݂ΏۂłB X͂̕K݂2d͔g̉͂A Ă^邱ƂŁA 萸ɍsƂ\ɂB w4 ֍u(4232)

### _wRLEifqj

 2014N0513i΁j16F4018F10 S c iwj uHolographic description of a quantum black hole on a computerv The discovery of the fact that black holes radiate particles and eventually evaporate led Hawking to pose the well-known information loss paradox. This paradox caused a long and serious debate since it claims that the fundamental laws of quantum mechanics may be violated. A possible cure appeared recently from superstring theory, a consistent theory of quantum gravity: if the holographic description of a quantum black hole based on the gauge/gravity duality conjecture is correct, the information is not lost and quantum mechanics remains valid. However, the duality has not been tested at the level of quantum gravity for more than fifteen years since its proposal. In this seminar we do it for the first time on a computer. The black hole mass obtained by Monte Carlo simulation of the dual gauge theory reproduces precisely the quantum gravity effects in an evaporating black hole. This result opens up totally new perspectives towards quantum gravity since one can simulate quantum black holes through dual gauge theories. (refs: arXiv:1311.5607(Science), 1311.7526(PTEP)) w4 ֍u(4232)

### _wRLEifqj

 2014N0428ij16F4018F10 q iwj u뎿ʍKXs܂ފgꂽ̗̏_̍\v {\IJ̏ԋԂne\ς ̏ۂƂɂA ̗̏_뎿ʂɔCӂ̍KXs_ igꂽ̗̏_j ̎Rȍp\ł ƂA̐c_B ̗_́Ȁ̗_Ɠ̃Q[WΏ̐߁A Ώ̐Gȏꍇɂ͈ʂɍł KXsQ[W̃Q[Wsύp̕ՓIȍ\ eՂɂƂ_B ƂāA ̓Iɂ̍KXsQ[W̍p\B ɁAtF~I܂ޏꍇւ̊gA ݍp܂ޗ_ւ̊g\ɂĂc_B w4 ֍u(4232)

### _wRLEiFj

 2014N0422i΁j16F4018F10 Z iHƑwj u_Xg̒ڍ̐ɂXfv f͘f_ɂő̓̂PłB X́AXq̕t̂̑fߒlɓꂽ f̓vV~[V𐢊Eɐ삯čsA Xf̌ɑ΂Ă f̂Q肪邱Ƃ𖾂炩ɂB w4 ֍u(4232)

### _wRLEifqj

 2014N0415i΁j16F4018F10 Ci iwj uJCΏ̐ƕ߁v Schwinger-DysonƓ암-Jona-Lasiniofg JCΏ̐̔jƉ񕜂ɂĂ̊{IȓeƁA NH[N̕߂Ɋ֌WbЉB w4 ֍u(4232)

## 2013Nx Hw

### _wRLEifqj

 2014N0121i΁j16F4018F10 󗘁@ iwj uLO-e\̌̏ɂāv ̑Ώ̐̓LOxNgɂċLqB ALO-e\݂̑ ̉BꂽΏ̐Ƃ΂BāA 炪LOxNgƓ悤ɁA Ȃ̗lXȏ̉^Ɋւۑʂ ڂɊ֌WĂ邱ƂmĂB {ȗOł́AJ[ubNz[ɁA LO-e\̈ʓIɂĘbB {ǔ㔼ł́A LO-e\̌̏ɂĘbB ACV^CȂǂĈʂɗ^ꂽ LO-e\ǂ͓łB LO-e\̍l@ɂA ̌ɏ邱Ƃ Semmelmann (2002) ɂĎꂽBŋ߁AXSemmelmanňʂpA 萸x̍^𓱂̂ŁA ɂĎԂĐB w4 ֍u(4232)

### _wRLEifqj

 2014N0114i΁j16F4018F10 iKIASj uNon-Lagrangian Theories from Brane Junctionsv We use 5-brane junctions to study the 5 dimensional (5D) T_N theories. These theories are interpreted as 5D uplift of the 4D N=2 strongly coupled superconformal theories which are obtained by compactifying N M5 branes on a sphere with three full punctures. Even though these theories have no Lagrangian description, by using the 5-brane junctions proposed by Benini, Benvenuti and Tachikawa, we are able to derive their Seiberg-Witten curves and Nekrasov partition functions. For T_3, we show that the Seiberg-Witten curve and superconformal index agree with those for Sp(1) theory with 5 flavor. w4 ֍u(4232)

### _wRLEiFj

 2014N0107i΁j16F4018F10 R Ti iF{wj u[vd͗_̊{ƌv d͂ʎq_IɋLq鎎݂̂PƂāA [vd͗_܂B [vd͗_܂pȂΏۂɁA ̗_Ȃǂ܂ɏЉA ŌɌɂĂȒPɂbł΂Ǝv܂. w4 ֍u(4232)

### _wRLEiFj

 2013N1217i΁j16F4018F10 ēc iswj uqA̍̂ƓdgΉV́v AqubNz[EqA̍̂ LIGOAVIRGOAKAGRA ̂悤 d͔g]̍łL]ȏd͔głB d͔gŌoꂽꍇAmMA 邢͏d͔g̐[mɂ́A dgΉV̂ɂϑ]܂B {Z~i[ł́A L]Ƃdgˋ@\ ɑ΂ŋ߂̌ʂЉB w43K 4340

### _wRLEifqj

 2013N1210i΁j16F4018F10 { Km iw^wj uQ[Wd͑ΉQCDEnhwւ̉pv ≏̂ɑ傫ȓdƁA≏j󂪔B QCDłłANH[N͉דdĂ邽߁A QCD^ɑ傫ȓdƁA≏łnh NH[NNH[N΂B ́AQEDł̃VCK[@\Ɠl̕ۂł邪A QCD̏ꍇNH[Nɂ͕ߗ͂L_قȂB ۓIQCDŃVCK[@\𖾂邽߁A AdS/CFTΉpĒΏQCDŐ^s萫vZB ʂ͕Iɉ߂łẢ܂߂čusB w43K 4340

### _wRLEiFj

 2013N1203i΁j16F4018F10 R ˕F iGlM[Ȋwȁj u21cm˂̊ϑɂj[gmʊKw\̐v j[gmʂ̗lȉF̍\ɉe^p[^́A CMB̊ϑɂ萧邱ƂłB ̂悤ȊϑƂċߔNڂĂ̂A 21cmƌĂ΂dg𗘗pϑłB {Z~i[ł́A21cmϑ̊TvƁA j[gmʊKw\A 21cmϑɂ菫ǂ̒xł邩ɂāA Xs͂̌ʂbƎvD w43K 4340

### _wRLEifqj

 2013N1126i΁j16F4018F10 [J p iwj uAnomaly or symmetry ?v ɂʎqF͊w(QCD)ł́AIɔjĂ SU(2) aJCΏ̐񕜂ƍLMĂ邪A U(1) ̃JCΏ̐ɂĂ ͂肵_ĂȂB ́ABanks-Casher ֌WgA SU(2) Ώ̐̉񕜂 Dirac Zq̌ŗLlz֗^鐧􂢏oA ɂ̌ŗLlz̐A U(1) Ώ̗̐Lɗ^e͂B ̌ʂ́ASU(2) Ɠ U(1) Ώ̐񕜂\ĂB {uł́Ả͂̊TvсA ܂ł́iΏ̐𑹂ȂōsĂj s̖_c_B w4 ֍u(4232)

### _wRLEiFj

 2013N1112i΁j16F4018F10 ΋@_ iߋEwj uAdS black holes and DC conductivityv 悸AAdS ̕s萫Ɠٓ_̔ɂ ŋ߂̗Tς܂B AdSł̃ubNz[Ƒo΂ ̋E_ɂDCɂāA iq\̌ʂꂽʂɂ c_Ǝv܂B w4 ֍u(4232)

### _wRLEiFj

 2013N1022i΁j16F4018F10 F_@mI iIPMUj uHigher spin ubNz[Ƃ̃Ggs[ɂāv higher spin _́A XsQȏ̗뎿ʏ(higher spin)܂ޏd͗_łB ߔNAhWb^[ԏhigher spin _ƁA ̋EŒꂽ̗_iCFTjƂ̊Ԃ̑oΐڂW߂ĂB Sȏłhigher spin̉^͕GɂȂA ̍p͈ʂɂ͒mĂȂB Rł́A̗_chern Simons _ƂċLqł邱ƂmĂB ̂Rhigher spin_ɂubNz[ (higher spinubNz[) ƂCFTIȉ߂KrausɂďڂׂĂB ɏdvȂ͎̂̌vʂhigher spiñQ[Wϊɂ 񎩖ɕωĂ܂߁A ۂ̒nʂhigher spin_ɂăQ[WsςȊTOł͂ȂƂłB ]ĒʏBekenstein Hawkingi邢͂̊głWaldj ̃ubNz[ɓĂ͂߂邱Ƃ͂łȂB ŉX͐Iٓ_@Chern Simons _ɓKp邱Ƃ Q[WsςȃGgs[𓾂B ͔̌M͊w@𖞂A ɑo΂ȏ̗_̌vZʂČ邱Ƃ킩B ̔\ł́ǍʂƁǍ̐iWɂăr[B w4 ֍u(4232)