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## RLE(2020NxȑO)

### _wRLEiFj

 2021N126i΁j16F3018F00 { iVj uEHTɂubNz[̎Bƍ̓W]v Event Horizon TelescopeiEHTj́Aۋ͂ɂnK͂̃~gVLBIϑԂ\zAubNz[̏ڍׂȎBڎwۃvWFNgłB2019N4AEHTvWFNg̏ʂƂāAȉ~M87̒Sɂ鋐ubNz[̎ʐ^JꂽB̉摜ɂ́Aqɑ郊OƃubNz[VhEʂĂAM87̒Sɑz65{̎ʂubNz[݂邱Ƃ炩ɂȂB{uł́AEHT2019N̏ʂɂĉ͎@摜瓾M87̃ubNz[̕ȂǂɂďЉƂƂɁǍ̐iэ̓W]ɂĂqׂB { IC

### _wRLEifqj

 2021N119i΁j16F3018F00 v iOOwj u􉽗_ɂ錷wiv 􉽗_͌_̔ۓ_I莮̈̌łB܂A􉽗_̒ɂĕKB􉽗_́Al̂̈̃NXł錷l̏̏d͗_łBɌl̏̔Cӂ̏d͗_ɂāARwi܂̃j[gɌƂƁAR̒_̑SI[_[̐ۓ_Č邱ƂB܂A10d͔wi􉽗_̏̔zʂɊ܂܂Ă邱ƂB̔zʂ͌􉽎ԂɈ˂Ȃ߁AGlM[邱ƂłBd͗_̉^𖞂wĩGlM[ŏwi肷ƂȂBwi肳΁Â܂̂炬W͌^oA𒴂ۂ̗\𓾂邱Ƃ҂B { IC

### _wRLEiFj

 2021N112i΁j16F3018F00 gc i_ˑwj ucFɂ鏉ٓ_ɂāv {uł́Aٓ_ւ̃{gAbvIAv[łȗ_̏ٓ_ւ̉pЉ܂BɁAcFɑ݂ٓ_̍\ƂāAFc̎w֐̂ɋNȗٓ_ƉF̔񎩖ȃg|W[ɋNٓ_ЉAȗ_Ƃ̊֘Ac_܂B { IC

### _wRLEifqj

 2020N1222i΁j16F3018F00 v h iswj "Fermi gas approach to general rank theories and quantum curves" Three-dimensional N=4 superconformal Chern-Simons theory described by circular quiver diagram is interesting because, for example, it can be considered to be the worldvolume theory of M2-branes. The partition function on S^3 can be reduced to a matrix model by using so-called supersymmetric localization technique. However, it was still difficult to study the matrix model non-perturbatively. To overcome this difficulty, a technique was developed to rewrite the matrix model into the partition function of ideal Fermi gas. This technique is called Fermi gas formalism (FGF). The FGF was applied to the circular quiver theories where all nodes have the same ranks. On the other hand, it was nontrivial whether the FGF could be applied to theories with different ranks. In this talk, we show the result of FGF for general rank theories. We also discuss the applications of our results. For example, the Hanany-Witten transition predicts that some matrix models are equal, and our result can be used to show the equality. We also show other non-trivial relations. Another application is that the relation between the matrix model with rank deformations and a quantum curve became clear. This is an extension of the relation in the absence of rank deformations. { IC

### _wRLEiFj

 2020N1215i΁j16F3018F00 ؓ i}bNXEvNd͕wj uAq̂̐lfǑƍ̓W]v d͔gCxgGW170817ɂďd͔g܂ރ}bZW[V̕w{iIɖJBAq̗̂_f̍\źAϑ\yщ߂Ŗ{IȖʂBɐlΘ_ƌĂ΂鐔lV~[Vɂ郂fO͕KvsłB}bNXvNd͕wComputational Relativistic Astrophysics division̖͂ɒNgłB{ułGW170817yѕtdgϑ̃r[A_fǑAW]ɂďЉ\łB { IC

### _wRLEifqj

 2020N128i΁j16F3018F00 Έ M iswj "Resonating AdS soliton" Non-stationary oscillating geometry can be obtained by nonlinearly extending normal modes in asymptotically AdS space. In this talk, I will construct what I call the resonating AdS soliton as the nonlinear extension of the modes dual to spin-2 glueball excitations of the AdS soliton. In particular, in five dimensions, I obtain the solution as a cohomogeneity-1 metric. It is shown that the holographic stress energy tensor of the resonating AdS soliton is time periodic, which is interpreted to give a coherently excited state in the dual field theory. The energy of the resonating AdS soliton is found to be higher than that of the undeformed AdS soliton, in accordance with the positive energy conjecture proposed by Horowitz and Myers. This talk is based on arXiv:2006.12783. { IC

### _wRLEiFj

 2020N123i؁j17F10~18F50 c Y i_ˑwj uANVInHzd͔gv ŋ߁ANANOGravϑ[A̕s̐MϑƔ\B ̐MANVIÍ̐Mł\c_B ANVI̎ʂ10^{-14}GeVł΁A傤nHzd͔gɑΉ邱ƁA ANVI̕萔10^{17}GeVł΁ANANOGrav̊ϑł邱ƂB _IɎRȕ萔10^{16}GeV̏ꍇł SKAϑŊϑ\ȑ傫̉~΋ɏd͔g邱ƂB { IC@iuɂ͎Oo^KvłB₢킹 tsutomu rikkyo.ac.jpj

### _wRLEifqj

 2020N1117i΁j16F3018F00 v iÉwj "On exact-WKB analysis, resurgent structure, and quantization conditions" There are two well-known approaches to studying nonperturbative aspects of quantum mechanical systems: saddle point analysis of the partition functions in Euclidean path integral formulation and the exact-WKB analysis based on the wave functions in the Schroedinger equation. In this work, based on the quantization conditions obtained from the exact-WKB method, we determine the relations between the two formalism and in particular show how the two Stokes phenomena are connected to each other: the Stokes phenomenon leading to the ambiguous contribution of different sectors of the path integral formulation corresponds to the change of the gtopologyh of the Stoke curves in the exact-WKB analysis. We also clarify the equivalence of different quantization conditions including Bohr-Sommerfeld, path integral and Gutzwillerfs ones. In particular, by reorganizing the exact quantization condition, we improve Gutzwillerfs analysis in a crucial way by bion contributions (incorporating complex periodic paths) and turn it into exact results. Furthermore, we argue the novel meaning of quasi-moduli integral and provide a relation between the Maslov index and the intersection number of Lefschetz thimbles. { IC

### _wRLEiFj

 2020N1110i΁j16F3018F00 ēc _ i哯wj u͌nS̋ubNz[ɂd͗_/ubNz[̌؁v X̋͂̒Sičjɂ́Cdg Sgr A*ičAX^[jmFĂB̎̐XiS-starsj̉^̑肩CSgr A* ͎ʂz̖400{̋ubNz[ƋĂBi̎̑IȐԊOϑC2020Nm[x܂50łBj S-stars ̒ S0-2 ƌĂ΂鐯i]16Nj́C2018N5 Sgr A* ŋߓ_ʉ߂B 2014N炷΂]S0-2̃j^[ϑ𑱂ĂC2018N̑f[^̓j[gd͂ł͐ȂƂ𖾂炩ɂłij[gd͂͋pꂽjB݁CS0-2̑f[^ɍłvd͗_c_邽߂ɁCvʂ Parametrized post-NewtoniPPNjWJ̕@ŏd͗_̃eXgixCYv́j{łB ̔\ł́CSgr A* ɂ܂錤̊TvЉCPPN eXg̐i󋵂񍐂B { IC

### _wRLEifqj

 2020N1027i΁j16F3018F00 ] iIPMUj "The O(N) model with ^6 potential in R^2~R^+" In this talk I will argue the large N limit of the O(N) model with classically marginal ^6 interaction in three dimensions in the presence of a planar boundary. This theory exhibits an approximate conformal symmetry at large N, then we can treat it as Boundary Conformal Field Theory(BCFT). Taking the advantage of this fact, I will compute large N effective potential, two-point functions of the conserved current and the stress energy tensor, which allow us to determine boundary anomaly coefficients in the trace of the stress tensor. I will then consider bulk and boundary conformal block decomposition of two-point functions. Finally I will explain how anomaly coefficients depend on quasi-marginal ^6 coupling. This talk is based on a collaboration with Christopher Herzog. { IC

### _wRLEifqj

 2020N1013i΁j16F3018F00 [J p iwj "A physicist-friendly reformulation of the Atiyah-Patodi-Singer index" The Atiyah-Patodi-Singer index theorem describes the bulk-edge correspondence of symmetry protected topological insulators. The mathematical set-up for this theorem is, however, not directly related to the physical fermion system, as it imposes on the fermion fields a non-local and unnatural boundary condition known as the "APS boundary condition" by hand. In 2017, we showed that the same integer as the APS index can be obtained from the eta invariant of the domain-wall Dirac operator in four-dimensional flat space. Recently we gave a mathematical proof that the equivalence is not a conincidence but generally true on any even-dimensional curved manifold. This talk is based on the following papers, Fukaya, Onogi, Yamaguchi, PRD96(2017) no.12, 125004 [arXiv: 1710.03379] Fukaya, Furuta, Matsuo, Onogi, Yamaguchi, Yamashita, arXiv:1910.01987 (to appear in CMP) Fukaya, Kawai, Matsuki, Mori, Nakayama, Onogi, Yamaguchi, PTEP 2020 (2020) 4, 043B04 [arXiv:1910.09675]. { IC

### _wRLEiFj

 2020N106i΁j16F3018F00 rc u iSapienza University of Romej "No-hair theorem and spontaneous scalarization of BHs" ߔNA񎩖ȃXJ[ubNz[(BH)@\ƂāABH̎IXJ[ƌĂ΂錻ۂڂĂBIXJ[NBH̎ɂ̓XJ[ꂪ񎩖ȔzʂB {uł́Aђ藝ЉɁABH̎IXJ[ɂčŋ߂ B { IC

### _wRLEifqj

 2020N929i΁j16F3018F00 V c iswj "Generalized Giveon-Kutasov duality" {uł͂RΏChern-SimonsQ[W_ɊւoΐuGiveon-Kutasov dualityv ̈ʉЉBQ[WQU(N)̏ꍇAChern-Simonsʉ邱ƂłASU(N)Q[WQɑ΂oΐ܂Ŋ܂񂾑oΐ̓IȋLq^邱ƂłB̗_ɂAʎq_IN[̎舵Aoΐ̌؂sBŌɁAʉꂽGiveon-Kutasovoΐ̉pЉB { IC

### _wRLEifqj

 2020N721i΁j16F3018F00 ȁ@l iHƑwj "Half-hypermultiplets and incomplete/complete resolutions in F-theory" I will talk about resolutions of codimension-two enhanced singularities from SO(12) to E7 and E7 to E8 in six-dimensional F-theory compactifications, where half-hypermultiplets arise for generic complex structures achieving them. The exceptional fibers at the enhanced point exhibit different structures depending on how the colliding 7-brane approaches the stack of gauge 7-branes, as previously observed by Morrison and Taylor in the case of the enhancement from SU(6) to E6. When the colliding brane approaches them as O(s), where s is the coordinate of the base space along the gauge 7-branes, the resolution process ends up with fewer exceptional fibers than naively expected from the Kodaira classification, with a non-Dynkin intersection matrix including half-integral intersection numbers. We confirm that the exceptional fibers at the enhanced point form extremal rays of the cone of the positive weights of the relevant pseudo-real representation, explaining why a half-hypermultiplet arises there. By altering the ordering of the singularities blown up in the process, we obtain, for both SO(12) -> E7 and E7 -> E8, the intersection diagram on every other row of the corresponding box graphs. We present detailed derivations of the intersection diagrams of the exceptional fibers at the singularity enhanced points by examining how an exceptional curve is lifted up on the chart arising due to the subsequent blowing-up process. When the colliding brane approaches the stack of branes as O(s^2), we obtain additional conifold singularity at the enhanced point, which completes the full Dynkin diagram of the enhanced group as was found previously. This talk is based on a collaboration with Shunfya Mizoguchi and Taro Tani. {(Japanese) IC

### _wRLEiFj

 2020N77i΁j16F3018F00 q _ iHƑwj "Scaled-up Electroweak Baryogenesis" ̃Z~i[ł́AXlĂfqW͌^𒴂VȖ͌^ЉA̖͌^ŎoI̋@\ɂċc_B܂A̐V͌^ւ̉̐Aꎟ]ڗȐd͔gϑɂĂAԂ̋c_sB We propose a new framework that a phase transition associated with a gauge symmetry breaking occurring (not far) above the electroweak scale sets a stage of baryogenesis similar to the electroweak baryogenesis in the Standard Model. A concrete realization utilizes the breaking of $SU(2)_R \times U(1)_X \rightarrow U(1)_Y$. New chiral fermions charged under the extended gauge symmetry have nonzero lepton numbers, which make the $B-L$ symmetry anomalous. The new lepton sector contains a large flavor-dependent CP violation, similar to the Cabibbo-Kobayashi-Maskawa phase, without inducing sizable electric dipole moments. A bubble wall dynamics associated with the first-order phase transition generates a $L$ asymmetry, which is transferred into a $B$ asymmetry via the ordinary electroweak sphaleron process. Unlike the Standard Model electroweak baryogenesis, the new phase transition can be of strong first order and the new CP violation is not significantly suppressed by Yukawa couplings, so that the observed asymmetry is easily realized. The model can be tested by the interplay of collider searches and gravitational wave detections. {(Japanese) IC

### _wRLEiFj

 2020N72ij15F2017F00 s ikwj uubNz[̋NFI~ɂ鋐启̌v X̋͌n͂߁Ax傫ȋ͂̒Sɂ͑zʂ100{ 10{x̋ubNz[݂Ă邪A̋N͓ɕ܂ĂB FaA10NɖȂɂĂ̂悤ȋubNz[ Ă邱ƂAubNz[̋N͉FɂA ƂȂubNz[̐ԂZƂAŏ̎펿ʂʏ Ƒ县ʂȂ̂]܂ƍlB {uł́Â悤ȑ县ʂ̎ubNz[ƂčlViI TςŁAŋ߁AX񏥂uI~vɂ鋐启̌ ̏d͕ɂubNz[ߒڏqB܂ŎnKX Ȋł͋启ꂦ邱Ƃ͒mĂÂ悤Ȋ ɂ߂ċHłA͒SɕՓIɑ݂鋐ubNz[̎ƂĂ ȂBAȌƎ˂̂̂ł̔ʂ̏df܂ނ悤ȃKX ߒ𐔒lV~[VƂAKX̕ɂ萯cA \鐯͋IɎ͂̃KXlĐ̂́Ał傫Ȑ ̒Sɑ݂āAقړƐIɑ葽̃KX~ĐA 10zʈȏ̋ȐƂȂd͕󂷂邱ƂB̂悤ɋ ÓAʏAʂ̏dfĂƂ񂪂A nKX̏ꍇɔׂđ̎ubNz[𐶐łƗ\zB {(Japanese) ICiOo^KvłB₢킹Fharada rikkyo.ac.jpj

### _wRLEifqj

 2020N630i΁j16F3018F00 { iswj "Digital Quantum Simulation of the Schwinger Model with Topological Term via Adiabatic State Preparation" I am going to talk about application of quantum computation to numerical simulation of quantum field theory. Specifically we implement a digital quantum simulation of a gauge theory with a topological term in Minkowski spacetime, which is practically inaccessible by standard lattice Monte Carlo simulations. We focus on 1+1 dimensional quantum electrodynamics with the -term known as the Schwinger model. We construct the true vacuum state of a lattice Schwinger model using adiabatic state preparation which, in turn, allows us to compute an expectation value of the fermion mass operator with respect to the vacuum. Upon taking a continuum limit we find that our result in massless case agrees with the known exact result. In massive case, we find an agreement with mass perturbation theory in small mass regime and deviations in large mass regime. We estimate computational costs required to take a reasonable continuum limit. Our results imply that digital quantum simulation is already useful tool to explore non-perturbative aspects of gauge theories with real time and topological terms. This talk is based on a collaboration with Bipasha Chakraborty, Taku Izubuchi, Yuta Kikuchi, Akio Tomiya. {(Japanese) IC

### _wRLEifqj

 2020N616i΁j16F3018F00 ۉȁ@G iwj "An application of quantum logic to quantum field theory" Formal-logical approaches to quantum physics originate from the work of Birkhoff and von Neumann in 1936. Since then, these kinds of approaches have been studied in mathematics, physics, logic, and philosophy. In this talk, we first sketch research backgrounds of this area, and introduce our motivations. Then we talk about our recent work, gDynamic Logic of Quantum Field Theoryh [2002.12203]. If time allows, we shall present further research topics in which we are interested. {(Japanese) IC

### _wRLEiFj

 2020N69i΁j16F3018F00 ߐ q iw Fj ud͔gŒTFNV́v d͔gϑ̃C^[Qbg̓RpNgÂłB̂܂ł̃^CXP[͐NFNȏƔɒ߁AFɂłAd͔gŊϑ邱ƂŉF̐i𖾂炩ɂł邩ȂB{\ł㐯NAubNz[̎ʁAXsAϑƏϑɂċc_B {(Japanese) IC

### _wRLEifqj

 2020N62i΁j16F3018F00 EM iÉwj "Towards elucidation of quantum criticality in the presence of quantum gravitational field" In statistical mechanics, a long-range correlation emerges due to a divergent fluctuation of a physical quantity and this is called the critical phenomenon. In particular, critical phenomena at the zero temperature are dubbed quantum critical phenomena because they are triggered by quantum fluctuations. In this talk, I will discuss quantum criticalities in the presence of quantum gravitational field. After explaining the motivation and the background of this study, I will introduce a particular model, the Ising model on 2d dynamical triangulations, and discuss its quantum criticality introducing an external parameter to the system and slightly modifying the underlying lattice structure. Then I will show that one can reach the quantum critical point with tuning the parameter to a certain value. As it turns out, physics at the zero temperature is quite sensitive about how we cool down the system. I will also show the existence of a continuous parameter that characterizes the way one approaches the quantum critical point and it may enter in a critical exponent. The talk will be based on Phys.Rev. D98 (2018) no.2, 026026 and arXiv:2003.08524 [hep-th]. {(Japanese) IC

### _wRLEiFj

 2020N526i΁j16F3018F00 c k iwrbOoFیZ^[j uFƂ (fq) F_Iہv FermiɂTeVu[U[̊ϑ͖{͂̃JXP[hGeVK}oĂȂB ͋͊ԂɎꂪƂΐłÂ悤Ȏ̋NFɋ߂邱Ƃ͋[\̈łB{uł́AF̓d㑊]ڑO(nCp[)ꂪꂽꍇNAfqIF_̊ϓ_ʔۂЉB ɁA(nCp[)ꂪwVeBĂȂ΁AfqW͌^̃JCʎqُʂāA d㑊]ڑOё]ڎɕΏ̂邱ƂɒڂB̋@\̂ɂ͑fqW͌^𒴂͕KvƂꂸAꐶɂW͌^zKvƂ̂łB{uł͂̋@\TA̍ՂƂĂ̋͊Ԏꂪǂ̂悤ȓׂЉBɁÂ悤Ȏ悤ȋ@\ƂāACt[VAAtbN_C@\AJCCs@\ЉB {(Japanese) IC

### _wRLEifqj

 2020N519i΁j16F3018F00 PT iwj "Nuclear states and spectra in holographic QCD" A new method to study nuclear physics via holographic QCD is proposed.Multiple baryons in the Sakai-Sugimoto background are described by a matrix model which is a low energy effective theory of D-branes of the baryon vertices.We study the quantum mechanics of the matrix model and calculate the eigenstates of the Hamiltonian. The obtained states are found to coincide with known nuclear and baryonic states, and have appropriate statistics and charges. Calculated spectra of the baryon/nucleus for small baryon numbers show good agreement with experimental data.For hyperons, the Gell-Mann--Okubo formula is approximately derived.Baryon resonances up to spin 5/2 and isospin 5/2 and dibaryon spectra are obtained and compared with experimental data.The model partially explains even the magic numbers of light nuclei, N=2, 8 and 20. {(Japanese) IC

### _wRLEiFj

 2020N512i΁j16F3018F00 u iwj "Testing gravity theories with cosmic microwave background in the degenerate higher-order scalar-tensor theory" {uł́AF}CNgwi˂̊ϑɂd͗_̌؂ɊւĂb܂BAłLNX̏d͗_łukލKXJ[Ee\iDHOSTj_ṽ{c}\o[ cmb2nd ւ̎܂̂ŁǍʂɂāA CMB ϑłǂ̒x̌؂\ł邩c_܂B {(Japanese) IC

### _wRLEifqj

 2020N24i΁j16F3018F00 i l iwj uEntropy of the Janus interface in four-dimensional N=2 superconformal field theoriesv We construct an co-dimension 1 defect across which a coupling constant changes its value, called the Janus interface, in an four-dimensional N=2 superconformal field theories. We then define its entropy as a contribution to entanglement entropy and show that the entropy associated to the Janus interface is given by a ratio of partition functions with and without the interface. By using this fact, we compute the entropy of the Janus interface to show that it is proportional to a particular linear combination of analytically continued Kahler potentials, as conjectured in 1805.09981 by Goto and Okuda. This presentation is based on a work in progress with K. Goto, T. Nishioka, and T. Okuda. {(Japanese) wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2020N128i΁j16F3018F00 ɓ xq (cmw) uQCD^_̒ቷẍ̕v QCD͑ꌴvZłiqV~[Vɂ鐔lIɂÃnhʂ̍ČLx]ڂ̒萫IEʓIU镑̉𖾂ɂĐ߂ĂBȂA͕݂̐邱ƂɂLxʂ𖳎łꍇɌĂB LxɂQCD͒qɂČ̕nƂđ݂Ăɂ炸A_Iȗ͂Ƃ茻ۘ_I悭ĂȂB ̎ȗRL̑ꌴvZłiqV~[Vɂ́ALxɂƁuvƂ{Iȍ薢ɊSȒ莮Ȃ߂łB {(arXiv:1910.12425)ł́AJ[̎RxĂQJ[QCDl邱ƂŕAɒ̒ϐł_CNH[Ňpɉ邱ƂŁA vZɓuቷẍv̌vZs\ɂB āAቷ̈ɂ鑊}肵Aeɂg|W[̕ω𒲂ׂB ܂Ԃ΁AarXiv:1811.05708ɊÂA~Y_ɂ镪CX^gɂĂЉB { (Japanese) wr܃LpX4 2K w֍u(4232)

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 2020N121i΁j16F3018F00 ꎓ iRwj uF}CNgwi˂ւ̔ʁAɎd̓Yʂɑ΂VȃAv[v ϑZp̌ɂAF}CNgwiˁiCMBjɑ΂ʁiۓ_ł͉͂łȂʁjϑ͂߂ĂBɁAvȌʂłd̓YʂɂẮAKEXB[hΌƂʓL̃VOǐoɂɐĂB{Z~i[ł́ACMBɑ΂ʂ̂܂ł̉͂ϑɂĉ\Ȕ͈͂Ńr[Aʂ𓝈InIɉ͂邱Ƃł "curve-of-sighth Av[ɂďЉB܂ApƂėlXȔʂɂĐB[hΌ]B { wr܃LpX44K 4408

### _wRLEifqj

 2019N1217i΁j16F3018F00 Seyed Morteza Hosseini iKavli IPMUj uA story of black holes' microstatesv Ifll review recent progresses in counting microstates of stringy black holes in AdS spacetimes. The main tools in achieving an exact counting are holography and supersymmetric localization. Combining these two Ifll explain how to derive the Bekenstein-Hawking entropy, including its numerical factor, for different classes of AdS black holes. p(English) [ύX܂]wr܃LpX44K 4408 (Rikkyo univ. Ikebukuro campus, room 4408 4th foor Bldg.4)

### _wRLEiFj

 2019N125i؁j16F3018F00 { i}gwj u~~ՂуWFbgtˎC̗͊wV~[Vv ubNz[⒆qւ̃KX~́A͊jXAƂxRpNgV̂̃GlM[ƍlĂBȂA~i~~Ձj̍\KXõJjY͂悭킩ĂȂB{uł́AtˎC̗͊wV~[VgŐV̌ʂɂďЉB܂ACxgEzCYEeXR[vƂ̋͂ɂ鍡̌vɂĂGB { wr܃LpX43K 4340

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 2019N123i΁j16F3018F00 ㏰ T iّwj uRectangular W-algebras and dual coset CFTsv KXs̗_Maxwell_d͗_RɈʉ̂łB_ł͍Xs̏ꂪ܂܂ĂA̒GlM[ɌɂĂ̂悤ȗ_Ɗ֌WĂƐMĂB̍ہAʏ̍KXs_ł͒_Ɍ鎩Rx邱ƂłȂ߁ÅgKvɂȂBŒڂĂ̂s񉻂KXs_łAZqpĒ_̑SԂLqłƊ҂ĂB܂AKXs_łAdS/CFTΉ\ł邱ƂmĂA3̃fȂo΂2CFT̑傫ȑΏ̐p͂\łB ̃Z~i[ł́As񉻂3KXs_̑QߑΏ̐łArectangular W㐔ƌĂ΂㐔ƑΉRZbg͌^ɂĐAX̌ЉB { wr܃LpX42K ֍u(4232)

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 2019N1122ij13F2514F55 zK Y isYƑwj uq̍ŏʁv 2015NɘAnɂpT[PSRJ0453+1559̎ʂ肳ꂽB̊ϑÂ̓V()͒qł\B܂ÃVXed͔gϑŃzbggsbNłAqłB̊ϑɂĔ̒q̎ʂzʂ̂킸1.17{ȂƂ炩ɂȂAWIȐ̐i₻̏I̗ɑ傫ȖNB{Z~i[ł́Aq̍ŏʂǂ̂悤ȕɂČ܂ĂāẢ݂FɂWIȒqViIœŏʂɂċc_B { wr܃LpX43K 4339

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 2019N1119i΁j16F3018F00 ֖ O iBwj uEvidence for Weak-Coupling Holography from the Gauge/Gravity Correspondence for Dp-branesv Gauge/gravity correspondence is regarded as a powerful tool for the study of strongly-coupled quantum systems, but its proof is not available. An unresolved issue that should be closely related to the proof is what kind of correspondence exists, if any, when gauge theory is weakly coupled. We report progress about this limit for the case associated with Dp-branes (with general p, from 0 to 4), namely, the duality between the (p+1)-dimensional maximally supersymmetric Yang-Mills theory and superstring theory on the near-horizon limit of the Dp-brane solution. It has been suggested by supergravity analysis that the two-point functions of certain operators in gauge theory obey power law with the power different from the free-field value (for p other than 3). In this work, we show for the first time that the free-field result can be reproduced by superstring theory on the strongly curved background. The operator that we consider is of the form Tr (Z^J), where Z is a complex combination of two scalar fields. We assume that the corresponding string has the worldsheet spatial direction discretized into J bits, and use the fact that these bits become independent particles when string tension is zero. { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2019N1112i΁j16F3018F00 q iswj uF̓ٓ_̎舵Ɋւ̒āv FȁuԂubNz[̒ȂǁAFɂ͗lXȓٓ_݂\Bٓ_ōpUƁAقȍp瓾ꂽb₻̉́AӖȂ̂ɂȂƗ\zB̖ɑ΂A܂p̐vAp̒lȏꍇɂٓ_̉\ɂċc_B { wr܃LpX44K 4408

### _wRLEiFj

 2019N1029i΁j16F3018F00 h iwj uDƃXJ[h炬d͔gv {\ł́ADXJ[h炬Ȑd͔gɑ΂ė^eɂččlBɁAD˗Dւ̈ڂς̑OエэŒ̗h炬̔W𒍈Ӑ[lBāAŏIIɐd͔g̓̎̈ڂς̃^CXP[ɑ傫ˑ邱ƂB { wr܃LpX44K 4408

### _wRLEifqj

 2019N1015i΁j16F3018F00 _c C iswj uAxial U(1) current in Grabowska and Kaplanfs formulationv Recently, Grabowska and Kaplan suggested a non-perturbative formulation of a chiral gauge theory (arXiv: 1511.03649). This formulation consists of the conventional domain-wall fermion and a gauge field that evolves by the gradient flow from one domain wall to the other. In this talk, I will briefly review their formulation and some related works. I will also discuss the QCD axial U(1) current in the formulation. It is found that the naive definition of the current does not reproduce the axial anomaly because the current includes a contribution from the bulk. I will suggest the correct definition of the current. This talk is based on arXiv: 1705.01317. { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2019N108i΁j16F3018F00 V w iÉwj uF_IpgXJ[e\_̐v gXJ[e\_́ACMBAd̓YʁAяd͔g̊ϑgݍ킹邱ƂŁAʑΐ_̂ꂪ%̐xŐƊ҂ĂB{Z~i[ł́AϑIɌ̓Iȃf̐AщF_Iϑʂ̌vZ@Ƃ̉ۑɂċc_B { wr܃LpX4 4K4408

### _wRLEifqj

 2019N101i΁j16F3018F00 { ĈY icwj ud͂̔M͊wɂ镪zƌoHϕɂāv d̔MtԂEuclidoHϕpĒ zɂċLqłƐMĂBȂ ʑΘ_EuclidoHϕill-definedƂȂȂ߂ɂ ϕoH(񓯒l)ό{Ȃ΂ȂȂƂmĂB ̈וz邽߂ɂ͐ϕoH肵Ȃ΂ȂȂB {łd͂̔M͊w╪zAoHϕɂă[sA v̕zɂēꂽʂɂċc_B Đv̕zۂ̖_ɂĂqׂB { wr܃LpX4ف@2Kw֍u(4232)

### _wRLEiFj

 2019N924i΁j16F3018F00 c \ iHƑwj uvʃAtBd͂ƔS[Xg\v vʃAtBd͂́Ad͂̓ƗȎRxƂď]̌vʂɉAڑNp闝_̌nłBߔNAڑɂΏ̐ۂƁAKɂĖ{S[XgȂƂĂB{Z~i[ł́AvʃAtBd͂̊bn߁AɃXJ[e\_ɃS[XgȂƂB { wr܃LpX4ف@4K4408

### _wRLEiFj

 2019N716i΁j16F3018F00 iOOwj ud͔g̏d̓Yv d͔grŏd̂̋ߖTʉ߂ƁAƓlɏd̓Yʂ󂯂āA̔gύXB{Z~i[ł́Ad͔gƏd̓Y̊bn߂āAŐV̗_Ɗϑ̘bЉB { wr܃LpX10 X301

### _wRLEifqj

 2019N79i΁j17F2018F50 q iwHwj ugꂽ̗̏_ɂ鍂KXsQ[W_̉͂Ɖpv ugꂽ̗̏_v́Ȁ̗_̏ԋԂ𕡐pӂ邱Ƃɂ蓾뎿ʂɔCӂ̍KXs_łB̗_́Ȁ̗_Ɠ̃Q[W\߁Ae퍂KXsQ[W̋Lqyщ͂ɉpłB{uł́Agꂽ̗̏_ƂɊÂKXsQ[W̍p̍\TAKXs̈ʂ̃Q[WsϗʂƁíjǏAݍp̍\AɂXs2̏d̈قȂ\ւ̊gȂǂ̏Ƃɑ΂W]c_B { wr܃LpX4 4340

### _wRLEiFj

 2019N72i΁j16F3018F00 v _Y iswV̊jj uAq̂ƐlΘ_v ̐NAAq̂̏d͔gtdgۂɌon߂ĂAq̏ڍׂȐdfȂǐVȕɔ鎞オĂB̐M𐳂߂ɂ́Aϓ鋭d𔺂q̍̂𗝘_IɐmɉƂK{łAlΘ_͂̂߂̗B̎@łB{uł́A{̐lΘ_O[vsĂvŽʂ𒆐SɁAd͔gdg牽킩ĂЉB { wr܃LpX4ف@3K4340

### _wRLEifqj

 2019N621ij16F3018F00 C r i_ˑwj uConformal correlators in momentum space and cosmological applicationsv Recent studies in cosmology have shown that analytic properties of inflationary correlators, together with approximate conformal symmetry realized at the end of inflation, are crucial for probing new physics at the inflation scale. These cosmological applications have then boosted research activities on conformal correlators in momentum space. In this talk, after introducing motivations from the cosmology side, I will discuss analytic properties and symmetry constraints on conformal correlators in momentum space. In particular, I will discuss how to construct a crossing symmetric basis of four-point functions based on consistent factorization in analogy with scattering amplitudes. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2019N618i΁j16F3018F00 ɓ i_ˑwj u}OmpGHzяd͔gTv LIGOɂd͔gϑɂāA{iIȏd͔gVwX^[gBlXȏd͔gɑΉčLgтł̏d͔gϑ߂Ă邪Ȁd͔gϑł100MHzϑ\ȍōgłB {\ł́Ad͔g}Om(dq̏W)N邱ƂǍۂGHzт̏d͔gTɗpł邱ƂBɁA}OmǔʂQƂ邱ƂɂāA8GHz14GHz̏d͔gɐ^B { wr܃LpX10 X301

### _wRLEifqj

 2019N611i΁j16F3018F00 q iGlM[팤@\j uTopological order in the color-flavor locked phase of (3+1)-dimensional U(N) gauge-Higgs systemv We study a (3+1)-dimensional U(N) gauge theory with N-flavor fundamental scalar fields, whose color-flavor locked (CFL) phase has topologically stable non-Abelian vortices. The U(1) charge of the scalar fields must be Nk+1 for some integer k in order for them to be in the representation of U(N) gauge group. This theory has a Z_{Nk+1} one-form symmetry, and it is spontaneously broken in the CFL phase, i.e., the CFL phase is topologically ordered if k is not 0. We also find that the world sheet of topologically stable vortices in CFL phase can generate this one-form symmetry. { wr܃LpX10 X301

### _wRLEiFj

 2019N64i΁j16F3018F00 k ikwj unubNz[ɂ鏬K͍\21cmVOiv nubNz[͉FɂČÄ݂Í̌ƂȂ肤V̂łBɋߔNLIGOɂČoꂽrIdubNz[̘ÂłƂĒڂW߂ĂB{uł͌nubNz[ɔ|A\mCỶF_IAƂďK͍\21cmVOiɂċc_B { wr܃LpX10 X301

### _wRLEifqj

 2019N531ij15F2017F00 (Wu̍ŏIR}) ۋg ꒨ iwHwj uLandscape of Superconformal Field Theories in 4dv Classification of superconformal field theories (SCFTs) is an important question in theoretical physics. We would like to (partially) answer this question focusing on SCFTs in four dimensions realized in the fixed points of the renormalization group flow induced by certain deformations of "known" SCFTs. The deformations include all possible relevant deformations and F-term couplings to gauge-singlet chiral multiplets. By "known" we mean we know the superconformal index (a generalization of the Witten index) in enough higher order. With this knowledge our deformation program is well defined and produces various fixed points. As simple examples, we see the deformations of the N=2 Argyres-Douglas theory, and of N=1 supersymmetric SU(2) gauge theory coupled to an adjoint and two fundamental chiral multiplets. In particular, from the latter theory, we find 34 fixed points, which cover all the known (low central charge) SCFTs and the interesting unknown ones, and 36 candidate ixed points possessing unphysical operators, including one with (a, c)=(0.20, 0.22), that need further investigation. { wr܃LpX4 4340

### _wRLEifqj

 2019N528i΁j16F3018F00 c q iw fq_j uQ[Wd͑ΉɂQCDJIX̉́v Q[Wd͑Ή͂̔ȗlXȕɉpA_w̌ɂĉIȐiW𑣂ĂBQ[Wd͑Ή̓ɂĂ͖킩ĂȂƂBǂ̂悤ȏ̗ʎq_d͑o΂ɂĂ͋ߔNɋc_ĂAdvȗvf̈Ƃď̗ʎq_̃JIXڂĂB{ł͂̂悤ȔwiɐGA̗ʎq_̃JIXQ[Wd͑ΉɂʓIɕ]BQCD̕ʂł郁\̎ԔWɒڂÃJIXǂ̂悤ȋN猻ꂤ邩ЉB { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2019N523i؁j13F2515F05 z itNtgwj uFirst M87 Event Horizon Telescope Results: The Shadow of the Supermassive Black Holev The Event Horizon Telescope (EHT) has mapped the central compact radio source of the elliptical galaxy M87 at 1.3 mm with unprecedented angular resolution. These images show a prominent ring with a diameter of ~40 micro-arcsecond, consistent with the size and shape of the lensed photon orbit encircling the gshadowh of a supermassive black hole. The ring is persistent across four observing nights and shows enhanced brightness in the south. Here we consider the physical implications of the asymmetric ring seen in the 2017 EHT data. To this end, we construct a large library of models based on general relativistic magnetohydrodynamic simulations and synthetic images produced by general relativistic ray tracing. We compare the observed visibilities with this library and confirm that the asymmetric ring is consistent with earlier predictions of strong gravitational lensing of synchrotron emission from a hot plasma orbiting near the black hole event horizon. Overall, the observed image is consistent with expectations for the shadow of a spinning Kerr black hole as predicted by general relativity. If the black hole spin and M87fs large scale jet are aligned, then the black hole spin vector is pointed away from Earth. Models in our library of non-spinning black holes are inconsistent with the observations as they do not produce sufficiently powerful jets. We also briefly discuss the possibility of the alternatives to a black hole for the central compact object. { wr܃LpX10X301

### _wRLEiFj

 2019N521i΁j16F3018F00 W iwj uK}o[XgF̊bƍŋ߂̘bv K}o[Xg͉Fő̔ۂŁAbԂ琔\bԂ̓nĔȃGlM[K}ƕo錻ۂłBWIɂ͌pԂi\bxĵ́A̕ɂłubNz[WFbgAZpԁi2bȉĵ̂́AqǍɕWFbgNƍlĂB WFbgAˋ@\Ȃǂ͖̕𖾂ł邪A{Z~i[ł͂̊bȒPɃr[Ǎۂ̉F̗jɂӋɂčlĂ݂Bɍŋ߂̐iWAɏd͔gƓɌoꂽo[XgATeVK}̌oȂǂɂĂЉB { wr܃LpX10X301

### _wRLEifqj

 2019N514i΁j16F3018F00 r 扗 iHƑw@fq_j uFinite N Corrections to the Superconformal Index of S-fold Theoriesv Recently, Garcia-Etxebarria and Regalado constructed S-fold theories, which preserve twelve supercharges, in four-dimension. The remarkable features of the S-fold theories are that there is no marginal deformation and the non-perturbative effect is essential. That is why the S-fold theories have no Lagrangian description and we cannot use the localization technique to calculate the superconformal index in the finite N, where N is the number of background D3-branes. In this talk, we present a calculation method of the finite N correction to the index on the AdS side, by considering the fluctuation of D3-branes wrapping the non-trivial three cycle in AdS_5 ~ S^5/Z_k. The key idea is to consider the superconformal field theory on the wrapped D3-branes and we can compute the contribution of the wrapped D3-branes to the index. On the CFT side, these corrections can be interpreted as Pfaffian-like operators. We also see our formula gives correct results up to a certain order of the fugacity of the index for rank one and two cases by using the supersymmetry enhancement. Reference:1901.00023 and 1904.09776 {(Japanese) wr܃LpX10ف@X301

### _wRLEiFj

 2019N57i΁j16F3018F00 c @C iswj uRpNgV̂ɂg̎UȂ̔gwv ubNz[ȐȂǂ̃RpNgV̂ɂ͌tsȉ~O(UCO)݂Bi􉽌wj̓dlƁAUCO̊OɌꍇɂ͐\ʂȂǂ̔˖ʂȂAUCO͓̓̏ȂBg̎UlƔgʂɂUCȌ𓾂邱Ƃ\łƊ҂BŖ{ł̓RpNgV̂ɂg̎UigwIȏd̓YjlB \ł́A܂gwƊ􉽌ẘ֌WʂĔgwIȏd̓Yl铮@ɂďqׂBċȂ̔gẘbƐsɂẴr[B̌AX̍ŋ߂̌ʂƂāAUV̂ubNz[ASz\ʂA[z[ł邩Ug̃p[XyNg画ʉ\ł邱ƂB { wr܃LpX10ف@X301

### _wRLEifqj

 2019N423i΁j16F3018F00 ʉ KY isw bwj uA Generalization of the Entanglement Entropy and Holographyv We define a new information theoretic quantity called odd entanglement entropy (OEE) which enables us to compute the entanglement wedge cross section in holographic CFTs. The entanglement wedge cross section has been introduced as a minimal cross section of the entanglement wedge, a natural generalization of the Ryu-Takayanagi surface. In this talk, we first overview the motivation and review basic ingredients in order to define the OEE. Then, we explain some basic properties of the OEE. Finally, we explicitly compute the generalized entropy for mixed states in two-dimensional holographic CFT and see agreement with the entanglement wedge cross section. This presentation is based on 1809.09109 (to be published in PRL). { wr܃LpX10 X301

### _wRLEiFj

 2019N416i΁j16F3018F00 ؑ u iwj uParametrized Black Hole Quasinormal Ringdownv ubNz[Âɕod͔g quasinormal mode(QNM,ŗL)ł悭ߎ,̔gʑΐ_̗\ɂǂ̒x߂,ƂƂ珫Iɏd͗_֑΂ĐtƊ҂ł.ۂɂs߂ɂd͗_ʑΐ_YꍇɂǂQNMɂȂ̂\ߒmĂKv.{\ł,̏Cd͗_ӎ,d͔g̊bɑ΂Ĉʑΐ_̕␳ꍇ QNM ŨVXe}eBbNȌvZ@ɂċc_.͊ȒP̂߂ Schwarzschild ubNz[̃P[Xɕ␳ꍇ𒲂,X̕@pĂ̐šʂČo邱Ƃ. { wr܃LpX10 X301

### _wRLEiFj

 2019N37i؁j15F0016F00, 16:1517:15 J iϏqj uʑΘ_It˗AvZɂ~ł̃ubNz[EVhEv N̂ɓdgvϑɂAߖT͒SɂubNz[~̒ɌC[WłubNz[EVhEBe\BZ~i[ł́AubNz[~E~~Ղ̕Ɠd g̕ˋ@\ɂĐŁAߔN܂ł̃ubNz[EVhĚɂčuB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2019N122i΁j16F4018F10 { D iw nvOEbȊwj u񕽍tJnɂ鎞ԕiΏ̐̔jƗL̗_v ԕiΏ̐̓GlM[ۑɌтCƂ{IȑΏ̐̈łD̂ƂCԕiΏ̐̔jƓ悤ɂāCԕiΏ̐IɔjꂽuԌvƌĂ΂VKȗʎqԂߔNɂȂĒĂꂽ[1]ĎCtԂɂĂ͎Ԍ͐ȂƂNo-Go藝ꂽ[2]C񕽍tł͎ԕiΏ̐̔j͗lXȏʂŋN邱ƂmĂD{ł́C񕽍tQCDF_ȂǂŐ鎞ԕiΏ̐̔jƂɕt암ES[hXg[[hLqL_̏Љ[3]D [1] F. Wilczek, Phys. Rev. Lett. 109, 160401 [2] H. Watanabe, M. Oshikawa, Phys. Rev. Lett. 114, 251603 [3] M. Hongo, K. Suro, T. Noumi, A. Ota, arXiv:1805.06240 { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2019N115i΁j16F4018F10 { l iswbwj uExact solutions in modified gravity with higher derivativesv F̉c̋Lqыdɂd͗_؂̂߂̘ggƂāAK܂ރXJ[Ee\_ߔNɌĂBS[XgȂ_̍\z@AʑΘ_̉Ɠ̌vʂ̍\@AŏNIXJ[Ȃǂɂċc_B { wr܃LpX4 4412

### _wRLEifqj

 2019N18i΁j15F0016F40 ؑ T iKEK _Z^[j uF_̃ZNV̂郂fƂȂfv F_͈ʂɑȉ~t@Cu[VCalabi-YauԂɃRp NgB ɂaxio-dilaton$SL_2(\Z)$ monodromy莮\ƂȂB F_̊b𕜏KAXF_̃f\т̕IӖɂ ċc_B @ȉ~t@Cu[V̓ZNVƌĂ΂\ꍇƁAł ꍇB ꂼAZNV̂郂fAуZNV̂Ȃf ĂԁB ZNV郂f̏ꍇAZNV̏WMordell-WeilQƌĂ΂ QȂB ̌Q̍\U(1)Q[W̏oƂoBZNV̂ fɂ͗UQ[WQB ZNV̂ȂfłAȉ~t@Cu[V͑ȉ~t@Co[ƕ ̓_Ō鑽dZNVʂɂ͎B ̑dZNV̎UQ[WQ肷B 烂f̍ŋ߂̍\ɂċc_B @Ԃ΁AF-theory/heterotic strings̑oΐɒ莮 stable degeneration limitƌĂ΂ɌA nongeometric heterotic stringsƌĂ΂wẽNXƂ̊֘Aɂ c_B { wr܃LpX4 4404

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 2018N1218i΁j16F4018F10 iߍHƍwZj uMyers-PerryMaxwell̕ϐɂāv 4]ubNz[łKerrɂMaxwelld ۓɑ΂^ϐɂ邱ƂmĂB A]ubNz[łMyers-Perryɂ ̉^ϐɂƂɂ͐ĂȂB ŋ߁ALuninɂāAMyers-PerryMaxwellϐ A ̌AKrtous-Frolov-KubiznakɂA̕ϐMyers-Perrŷ Killing-YanoΏ̐ Ɗ֌WĂ邱ƂꂽB ܂A炩ƂȂ̕ϐ\ ܂ŒmĂϐ\Ƃ͈قȂ邱ƂA ݁Ad͐ۓɑ΂^̕ϐɂ܂ pł̂ł͂ȂƊ҂ĂB {uł́A܂4KerrMaxwell̕ϐ\ ȂMyers-Perryւ͓KpłȂ̂A čŋߔꂽϐ\Ƃ͂ǂ̂悤ȍ\Ȃ̂ɂăr[ A ŋ߂̉X̌łEinsenhart liftɂsymmetry operators̍\@ɂ ЉB { wr܃LpX4 4412

### _wRLEifqj

 2018N124i΁j16F4018F10 c iKavli IPMUj uPhenomenological Consequences of the Refined Swampland Conjecturev Recently, the swampland conjectures, which state that quantum gravity does not allow all field theory in IR, is drawing attention. In particular, Obied et al's de Sitter conjecture, 1806.08362, claims that the de Sitter spacetime is not consistent with the Quantum gravity. Since the de Sitter spacetime plays an important role in the cosmology, the conjecture is phenomenologically important and even falsifiable. We first review the conjecture and show various phenomenological problems which the conjecture causes. Then, based on our paper 1810.06532, we see the newly proposed conjecture 1810.05506 by Ooguri et al. solves some of them but still has tensions between the inflationary Universe. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2018N1127i΁j16F4018F10 c Y i_ˑwj uString Axion in the Skyv ANVI͈Í̌ł邾ł͂ȂAd͔g̏dvȃ\[XłB ANVIǂ̂悤ȕIȌۂ𐶂ݏôAgăANVȊ݂؂邱Ƃł̂ c_B܂AANVId͔g̕Ɣ@ɑlɌтĂ̂B { wr܃LpX4 4412

### _wRLEifqj

 2018N1116ij16F4018F10 xc ikwj uSoft-hair enhanced entanglement beyond Page curves in a black-hole evaporation qubit modelv We propose a model with multiple qubits that reproduces the thermal properties of four-dimensional Schwarzschild black holes (BHs) by simultaneously taking account of the emission of Hawking particles and the zero-energy soft-hair evaporation at the horizon. The results verify that the entanglement entropy between a qubit and other subsystems, including emitted radiation, is much larger than the BH entropy analogue of the qubit, as opposed to the Page curve prediction. Our result suggests that early Hawking radiation is entangled with soft hair and that late Hawking radiation can be highly entangled with the degrees of freedom of a BH, avoiding the emergence of a firewall at the horizon. { wr܃LpX 44340

### _wRLEiFj

 2018N1113i΁j16F4018F10 Bernard Carr iQueen Mary University of Londonj uPRIMORDIAL BLACK HOLES AND THE LEGACY OF STEPHEN HAWKINGv There is now overwhelming evidence for black holes of around 10-100 M_{\odot} as the remnants of stellar collapse and supermassive black holes of around 10^{6}-10^{10} M_{\odot} at the centres of galaxies. However, black holes may also have formed in the early moments of the Big Bang, as first suggested by Stephen Hawking and could span a much broader mass range. Although there is no definite evidence for such primordial black holes, they have been a focus of intense study because they are the only ones which could be small enough for Hawking radiation to be important, those lighter than around 10^{15}g having evaporated by now. Larger (non-evaporating) primordial black holes could also be important, possibly providing the dark matter or the black-hole mergers detected by LIGO or some features of cosmic structure. The speaker was Stephen Hawking's PhD student at the time of his discovery of black hole radiation and will include some personal reminiscences. p(English) wr܃LpX4 4412(Room 4412, 4th floor Bldg. No.4, Ikebukuro Campus, Rikkyo University)

### _wRLEifqj

 2018N1030i΁j16F4018F10 X r icmwj uBions and resurgence in CP^N modelsv Perturbation series in quantum field theory are generically divergent asymptotic series. Resurgence theory relates such perturbation series and non-perturbative effects which cannot be captured by the perturbative expansion. It has been shown that the so-called bion saddle points, which consist of instanton-antiinstanton pair, plays an important role in resurgence theory in a certain class of quantum systems. In this talk, I will overview the recent development of the resurgence theory based on the complexified path integral and the bion saddle points. As an example, I will talk about CP^N model and show that it is powerful enough to reproduce exact results from the perturbation series and semi-classical bion contributions in CP^N quantum mechanics. I will also talk about an extension to the 2d CP^{N ?1} models on R \times S1 with twisted boundary conditions and show that the semi-classical bion contributions is consistent with the expected IR-renormalon ambiguity. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2018N1023i΁j16F4018F10 Jose M M Senovilla iBasque U., Bilbaoj uWhat is the surface of a black hole?v Black holes are fundamental objects in equilibrium predicted by General Relativity. However, in reality, black holes form, evolve and eventually evaporate, thus they are dynamical. The boundary of a black hole is thus not well defined, as the usual Event Horizon is global and teleological. One can resort to using the local concept of closed trapped surface to try and define the surface of black holes, leading to the concepts of dynamical and trapping horizons. We will show the fundamental problems inherent to dynamical or trapping horizons. The trapped region and its boundary will then be introduced, and the difficulties in finding them highlighted. Finally, the concept of core of a black hole will be briefly discussed. p wr܃LpX4 4412

### _wRLEifqj

 2018N1016i΁j16F4018F10 isw wȁj uRegular solutions in a deformed Jackiw-Teitelboim modelv We study deformations of a particular (1+1)-dimensional dilaton gravity model, called the Jackiw-Teitelboim (JT) model, by employing the Yang-Baxter deformation technique. In a original frame, the deformation makes the spacetime structure around the boundary change drastically and a new naked singularity appears. However, by employing a Weyl transformation to the deformed model, we obtain a Liouville dilaton gravity model with a cosmological constant term. Then regular solutions can be constructed with coupling to a conformal matter by using SL(2) transformations. For a black hole solution, the Bekenstein-Hawking entropy is computed from the area law. This entropy can also be reproduced by evaluating the boundary stress tensor with an appropriate counter-term. { wr܃LpX4 ֍u(4232)

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 2018N109i΁j16F4018F10 c SY iÉj uʓIԂɂXgJXeBbNCt[Vv Ct[VɂdvȊϑʂ1ƂėʎqUR̃XJ[炬mĂ܂A ̂炬܂߂Ct[V͎̉@ƂăXgJXeBbNCt[VƂ܂B ̌ł̓XJ[炬ÓTIFmCYŋߎ܂A X͔FmCY̐wI̔CӐɋNāAXgJXeBbNɕsȕs萫݂邱ƂwEA tIɂ̕s萫̏XgJXeBbN̓KpÓ̐VȎwWƂȂ邱Ƃ񏥂܂B ܂XgJXeBbN̎pIȉpɂĂЉ܂B { wr܃LpX4 4412

### _wRLEifqj

 2018N102i΁j16F4018F10 {n ^H isw@bwj uTime Shifts via Double Trace Deformationsv Recent study by [Gao, Jafferis, Wall] has shown that by introducing double trace deformation, one can make non-traversable wormhole of two sided black hole traversable. In my talk, I will consider double trace deformation in pure global AdS, and study time evolution after turning on non-local double trace deformations. I will consider two kinds of double trace deformations, the first is composed of two local operators placed at different points in AdS boundary. The second is composed of two HKLL bulk local operators, modeling interacting black hole binary in AdS. In both cases, with suitable choice of sign of the deformation, creation of negative null energy shocks and violation of ANEC are observed. This implies that there is time advance in the bulk. We also compute time evolution of entanglement entropy and Renyi entropy. { wr܃LpX4 ֍u(4232)

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 2018N925i΁j16F4018F10 ؑ u iIST, University of Lisbonj uStability analysis of a black hole by S-deformationv Ώ̐̍ubNz[ɑ΂d͐ۓ̓VfBK[Ɠ̕ƂɋA邱ƂD{\ł͂̂悤ȏꍇɎ̈萫߂̊ȒPȕ@ĂC̕@͎󂪈ȂΏɓKp\ł邱ƂDɕIRxꍇւ̊gsD { wr܃LpX4 4412

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 2018N710i΁j16F4018F10 V Ďu iÉwj ud͔gdɂd͗_̌؁v ŋ߁AqÂ̏d͔goAK}o[XgƂ̓ԍd͔g̓dxɐɑ肳ꂽBɂȀCd͗_ɑ΂ċꂽBŁAd͒萔̎ԕωd͔gdɂƂĂdvȊϑʂłB{Z~i[ł́Ad͔gdɂd͗_̌ؕ@ɂďЉÅϑɂēd͗_ւ̐ɂĘbłB { wr܃LpX44K 4412

### _wRLEifqj

 2018N73i΁j16F4018F10 c ͎ iAIP/iTHEMSj uDeep Learning and AdS/CFTv Recently, machine learning techniques, in particular techniques of deep learning, are unprecedentedly developed.In deep learning, we prepare graphical systems with layered structures called multilayer perceptions (MLPs). MLP includes tunable parameters, and we fix them via some updating algorithm. It is called "training" or "learning" process in machine learning community. In our paper, we suggest an idea of deep learning/AdS correspondence by showing that a system of scalar bosons in AdS background can be mapped to corresponding MLP. In this context, all parameters of the bulk theory including coupling constants and background metric correspond to tunable/learning parameters of the MLP, and we can fix them through learning process by using the boundary data we want to explain. In this talk, I also explain basics of machine learning techniques focusing on MLP and related recent papers. { wr܃LpX4 ֍u(4232)

### _wRLEiFj

 2018N626i΁j16F4018F10 암 ے iÉwj uHarvesting Large Scale Entanglement in de Sitter Space with Multiple Detectorsv ʎq̎ʎqiG^OgjoP̕@ƂāCƑݍpQ̌oԂ̑ւp@D̕@ŃCt[VFɂʎq]ƁCnbunzXP[ŌoԂ̗ʎqꂪ؂邱ƂmĂD{ł́CRȏ̌opӂ̑ւ̌ʂl邱ƂŁCXP[ɂʎqꂪo\ƂȂ邱ƂĎʂ͗ʎq̎{Ił郂mK~[ɋND { wr܃LpX43K 4340

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 2018N619i΁j16F4018F10 n ^ iKavli IPMUj uThe Large Charge Expansion and the Universal Correlation Functions in Rank-1 SCFTv The two-point functions for generator O of Coulomb branch chiral rings in D=4 N=2 SCFT will be determined universally to all orders in 1/n by the theory's a-anomaly. The calculation will be done using the method of large-charge expansion presented in [1706.05743]; the absence of F-terms in the (R-charge)^(-1) expansion of the effective action ensures this universality. I will also comment on the non-universal and non-perturbative corrections to the two-point functions whose leading piece was numerically shown to go as O(exp(-sqrt(n))). { wr܃LpX4 ֍u(4232)

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 2018N614i؁j16F4018F10 M Ďj iswj u䂪񂾉F̑K͍\FF_̐Vv[uv ̓T[xCĊϑF̑K͍\́AF̐藧ƐiɊւMdȉF_I܂ł邪AhԕΈڋԘc݁hƌĂ΂ϑIȌʂɂČnIɂ䂪ŌBAߔNA̘c݂𑪒肷邱Ƃł́AF_IȑXP[ŏd͂eXgłƂđ傫Ȋ֐SW܂ĂB{Z~i[ł́Aّ͂̓xɂĈNuWIȁvԕΈڋԘc݂ɂăr[AΘ_IʂɂĐVȘc݂ɂċc_B ̘c݂̃j[Nȓ𒲂ׂ邽߁AΘ_IʂlV~[VJ^O쐬ẢeςʂɂďЉA̓ƌo\Ȃǂɂċc_B { wr܃LpX43K 4340

### _wRLEifqj

 2018N64ij16F4018F10 ۋg ꒨ iwj uRG flows and deformations of simple SCFTsv In this talk, we will explore possible RG flows of four-dimensional N=1 SU(2) gauge theory with adjoint and a pair of fundamental chiral multiplets (Nf=1) by relevant deformations. By these, we allow the ones by adding a free chiral multiplet M and coupling it to a chiral operator O by superpotential W = M O. Fixed points by these deformations can be studied by using a-maximization and superconformal index. We find there are two fixed points where N=1 supersymmetry is enhanced to N=2. These are indeed the Argyres-Douglas theories H_0 and H_1. The other fixed points are purely N=1 supersymmetric, including various new SCFTs. We will discuss some properties, eg chiral ring, of them. This talk is based on the collaboration with Emily Nardoni and Jaewon Song. { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2018N529i΁j16F4018F10 g iswj uODE/IM correspondence and its application to N=2 gauge theoriesv In this talk we discuss a mystery correspondence between the linear problem associated with affine Toda field equations and two-dimensional massive integrable models, which is known as the massive ODE/IM correspondence. Based on the $\psi$-system satisfied by the solutions of the linear problem, we derive the Bethe ansatz equations and determine the asymptotic behavior of the Q-function for large value of the spectral parameter. We then derive the non-linear integral equations for the Q-functions from the Bethe ansatz equations, and compute the effective central charge in the UV limit. If time is allowed, I will show several new results, when we apply ODE/IM correspondence to N=2 gauge theories. { wr܃LpX4 ֍u(4232)

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(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)

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 2018N515i΁j16F4018F10 iswj ud͔go̘A̓ہv ۂ͕Ȋŵ݂Ȃ炸wHwȂǂłLϑĂB{ułd͔go2̘Aɂč\KwI4̌n̐ic_B āÂ悤Ȍn𓯊Ԃֈނ߂̃JjYBɁAɎ鋻[VwIۂЉB { wr܃LpX4 4412

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

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 2018N51i΁j16F4018F10 rc u iÉj uMaximal Luminosity Conjecturesv Maximal Luminosity ConjecturéAF̗lXȕIȌno郋~mVeB[ɂ݂ƂłAGibbonsɂĒ񏥂ꂽB{uł́ẢȂ҂̂AǂقǕՓIɐ鉼Ȃ̂ɂāAvlʂċc_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)

### _wRLEiFj

 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)

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 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)

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 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)

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 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(dł̔g)̉ɁAK؂ȋE(BHŊO̐isgABHnʋߖTœ̐isg)ۂƂœBȂABHnʕt߂ɔI\݂BȂ΁AgPlanckTCYɂȂ܂ŏd͓IΈڂ󂯂̏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)

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 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)

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 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@ACFTȂԂɒꂽꍇɓKp̌ʂɂĂc_BԂ΁AHolographicԂ̃XJ[̓֐GlM[^ʃe\̌vZȂǂ̍ŋ߂̌ЉB { wr܃LpX4 ֍u(4232)

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 2017N1219() 16:40--18:10 n I iwj uԂɂ鎞Ԍ̔񑶍ݐv m[xܕw҂Wilczek2012NɒĂAȋc_̑ΏۂƂȂuԌvɂĐUԂBƂƊԂ╽tԂŋN蓾ƂꂽԌł邪AX̒Ăł͂uvmɂ͗^ĂȂBX͒ւƂꂩ̒^ÄӖł̎Ԍs\ł邱Ƃ̂ŁA̋c_ЉBߔNꂽOꒆɂ鎞ԌƂ̊֘AɂGB Ref: HW and Masaki Oshikawa, PRL 114, 251603 (2015) { wr܃LpX4 ֍u(4232)

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 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)

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 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\ɂĂc_B { wr܃LpX42K4232i֍uj

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 2017N1114() 16:40--18:10 ^ iswj uSachdev-Ye-Kitaev͌^ƃJIXv Sachdev-Ye-Kitaev (SYK)͌^2015NɒĂꂽA(0+1)ÑtF~I_4̑ݍpʎq͊wnłBN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 ͌^̌iqɕ߂pqnɂ[1]A (2) SYK ͌^ɂ钷Ԃ̑֊֐̐Uƃ_s̊֘A[2]A (3) SYK ͌^ɃtF~ĨzbsOɑ2̍ĕό nł̃JIẌ萫[3] ȂǂɂČi߂ĂB{uł́ASYK ͌^̌󋵂X̌̓@ɂĐƁA܂A(1)(2) ̌̊TvqׁAŁA(3) ɂďڂЉBԂ̗]T΁AɊ֘AĒׂĂAȇ厩RxÓTJIXñAvmtw̕z̋ʐ [4] ɂĂGꂽB [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)

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 2017N119 16:40-18:10 ΋ _iߋEj uBMSΏ̐Əd̓[v d̓[d͔g̔UIȌʂłARqnd͔go[Xgʉ߂ɎRq̑Έʒûꂪɖ߂炸܂łcƂAIɊϑ\ȌۂłBߔNÃ[ʂƎ̑QߑΏ̐Aѓd͎q3̊֌W炩ɂȂĂ܂B{Z~i[ł́Ad͔g[ʂƎBMSΏ̐ǂ̂悤ɌтĂ̂A4ƍ̏ꍇr܂B { wr܃LpX43K4340

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 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ۂɂĂc_B { wr܃LpX4 ֍u(4232)

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

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 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ŒĂꂽA̔W͉ϕ̗͂ɂƂ낪傫ϕpȂ@ɂĂ̗͖RB{ł́Ahexagonalization̊JłƂ߂ł1/2-BPS Wilson loopɑ}ꂽoperatoȓ֊֐ɒڂ邱ƂŁAWilson loopEƂđ݂邽߂ɕ̗̎ʂperturbationvZł̂ł͂ȂƊ҂A2̈قȂ錩łperturbationhexagonalization̑ΉɂČsĂB̍uł͂̌̌ɂĐB { 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߂ɂ͔lFfł̐ۓvZKvsłB {\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_ɊÂʎqAoCʎqُɋNAۂɂċc_D܂Cŋ߂̐iWɂĂЉ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_̂̐ɂāv 6ꗝ_͌݁Aɑ̗ႪĂ邪AOWAmĂ炸A̕I\ɉ𖾂ꂽƂ͌B{uł́A6ꗝ_̎̓IȐɂāAu҂̎ɂēꂽʂ𒆐SɉB܂A6ꗝ_̑\Iȍ\@𕜏KB̌A6_̃e\}ɌCX^g̐Eʗ_ɂāA̒Sdׂǂ̂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ł́ÅȒPȎʂȂA[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ő̏Q̂ЂƂƂĖ30NԂɂ킽ė͂ĂAŋ Neveu-Schwarz sector Ramond sector 𗼕܂ފJ̗̏_̃Q[Wsςȍp̍\ɐB͌ÓTIɊSȒ̗̏_̒莮̍ŏ̗łB܂ASen ͗]vȎR𓱓邱Ƃŕ̗̏_̃[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҂Ă̐ۂɖĂ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_ɂΏ̐̔jɂĒׂB̓Iɂ́Aۓ_𗘗p3ՊEO(N)͌^ɂ鍂Xs̃Jgُ̈펟ČB̏ŁAۓ_ɂvZo΂ȗ_̌tɖ|󂵁AQ[Wꂪʂ悤ɂȂdg݂ʓIɗBɁẢ͂o΂ȍXs̗_ʂ̗_ɊgA_Ƃ̊֌WɂĂc_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^JEiKɂčl@,ʑΘ_̌؁ECɂċc_. { 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]ɂĂc_B { wr܃LpX42K ֍u(4232)

### _wRLEiFj

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

### _wRLEifqj

 2016N1129i΁j16:4018:10 㓡 Đl iwȁj uoN̋ǏNԂʂČAdS̈ʍ\v AdS/CFT̋@\悭邽߂ɂƂdvȖ̈ƂAdS̋ǏCFTǂ̂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CFT̏ꍇAǏN̎ԔWd͑̈ʍ\𔽉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[̌̕ɂĊTςA̗_I 炭BSWʂɑ΂␳ɂċc_B { wr܃LpX42K ֍u(4232)

### _wRLEiFj

 2016N118i΁j16:4018:10 u iwj uField-theoretic simulations of cosmic stringsv FR͂āAK͍\̑fƂȂh炬 ̂ƂČɍsĂ܂A COBE q͂߂ƂlXȍx̉Fϑɂ ے肳邱ƂƂȂǍ҂̋̒S͊OĂ܂܂B AFR͓ꗝ_⃉hXP[vIȕł͕sȐ^̑] 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AɖAFm̏Փˌۂɂċc_ЉB { wr܃LpX42K ֍u(4232)

### _wRLEifqj

 2016N104i΁j16:4018:10 R N iwj uꗝ_̎@ɂA]Qtwist defect̗_̃ÓWJv twist defect ƌĂ΂A]QdefectiǏZqjɂčl@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znOfAɂ͊CΘf܂łĂ錻݁Aɐ݂Ă邩ǂm邽߂ɂ́ÃyCEu[Ehbgȏ̏oϑ@m邱ƂK{łBƂɍŋߔꂽvNV}P^E̎̊Θf́Ǎ̏̕dv̂łB @X́uЂƂ̒nv̎]ɑΉāÃhbǵuFvIɕω邱ƂɒڂĂBFϓp^[ǂł΁AЂƂ̒n̏ɂ嗤CA_݂̑𐄒ł͂BɁAł͗ΐFłn̐A̗t́AߐԊÖɂĕՓIɑ傫Ȕ˗ĂAÃbhGbWƌĂ΂ĂB܂AߐԊOŊϑΐA͂܂˂^ԂȂ̂B̒̐𗘗p΁AЂƂ̒n̐FωɍԂ̊AȂ݂m鎖ł̂ł͂ȂByCEu[EhbĝȃYo鎖ŁAFwւƂȂ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{uł߂ɁALxAxQCD̑}т̌ۂւ̉pTςBɁAQCDۓIɉ͂鋭͂Ȏ@łiqV~[Vɂ͗LxɂĕƌĂ΂鍢邱ƂA̍𗝉wWƂăVo[uCYۂB @u㔼ł́AfWo@ȒPɏЉɁAX̍ŋ߂̌Љ[1]BL͂Ȏ@ƂāAߔNAoHϕ̕fɊÂ̎@AfWo@уtVFbcVu@͓IɌĂBX͂̎@p1TCgno[h͌^ɂVo[uCYۂ͂[1,2]B{uł͓ɕfWo@ɂĂ̌ʂЉ[1]B܂AtVFbcVu@Ƃ̔rɊÂfWo@̉Pɂċc_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_֊֐𒲂ׁAϕȋꗝ_̏ꍇƂ͈قȂ錋ʂ𓾂BAʎq̌^ɂJIX̎wWƂėʎq̊h(XNuO)BRCFT̗łSU(N)k WZW͌^ɂāAXNuO̎wWƂċǏIɗNꂽԂ̃G^Og̎ԔW𒲂ׂB̌ʁASdׂ傫Ɍ邱ƂŁAϕȗ_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_̕\_͒jC̍s񎮁i2ꗝ_Kac̗ގj񏥁Eؖꂽ͍̂NɂȂĂłD͂̌̈ӖƉpC֘Aɂċc_D { wr܃LpX42K ֍u(4232)

### _wRLEiFj

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

### _wRLEiFj

 2016N614i΁j16:4018:10 ߐq펁iwj u㐯NAubNz[̏d͔gv 㐯30Msun̘AubNz[(BBH)ɂȂ茻݂܂ō̂ɎcĂ̂邱ƂB]XAŊϑꂽBHɔ3{xdBAd͔g̊ϑʂ͖30MsunBBĤłBAdBBH݂̑ĂA㐯NȂB { 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 ɂāAȒPȃr[̌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[gd͂ɂĂ͓IȈʉȂƂĂDC͂ĂCႦ΁COW̐Op͑znɂđΉV̂ĂDX́C̉ʑΘ_IdɂčČCP̃|XgEj[gߎ̂ƂőΉ镽t𓱏ôŏЉD萫Əd͔g˂ɔpɂO̐iɂĂc_D { wr܃LpX4 ֍u(4232)

### _wRLEifqj

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

### _wRLEiFj

 2016N419i΁j16:4018:10 ꕽ iswj uQ[W̌ʂŐJCȌnd͔gɂāv F̃Ct[VɃQ[WꂪANVIƋĂƁApeBΏ̐jd͔g𐶐邱ƂmĂBɁAQ[W̏ꍇd͔gxŐ邱Ƃł̂ŋ[B{ł́A̗lȃJCȌnd͔g̐@\ɂĐAϑ\ɂċc_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 ̂́jɂċc_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ɂĂc_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_̃ZbgɂĂ̘aƂēB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2015N1215i΁j16F4018F10 n l iswbwj u2ꗝ_ɂdǏZqɂNԂɂĂ̗ʎqƃXNuԁv ʎqnNɂ藐Ǎn̗ʎq̓IȐUc_悤ƂƂAʎqꂪ\̂͂Ɩ₤͎̂RȂƂł낤Bnɏ\ꂪACӂ̕nő̃G^OgEGgs[𓾂ƂAn̔ȏ̎RxɂĒmȂȀԂɂĂ̏𕜌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ǂdvȖłB{ułpp-waves͌^ł̖̕ߒc_B̉ߒ͂̃glʂƑBAdS/CFTΉʂABJM_Ƃ̊֌WȒPɋc_ÃglʂLqBPSCX^g͍sTCY傫ꍇ3̃vXƓɂȂ鎖BXɕߒLq邽߂ɂ́AʏR^3ł͂ȂARiemannʂ̗l2R^3\荇Ԃ̏ł̉KvȂƂBۂ̃vX̉gĎۂɖ􂷂p𑨂̃vbgBStefano 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

 2015N1020i΁j16F4018F10 {n ^H iswbwj uSurface/stateΉɂHolographÿʉƋǏIɗNꂽւ̉pv ߔNAdS/CFTΉɂʎqG^OǧɂA̗_̗ʎqG^OgƁAd͗_̎̊􉽂Ƃ̊Ԃɋ֌W邱Ƃ炩ƂȂBCFT猻d͗_̎́A^Ԃ̗ʎqG^Og􉽊wIɕ\e\lbg[NƂėoAƂwEȂĂB{uł́Ae\lbg[N̐ɒڂ邱ƂŁA̗\zE̖ɂʉo邱ƂB܂A_Nꂽɑ΂Ă̈ʉǂKp邩qׂB { wr܃LpX4 ֍u(4232)

### _wRLEifqj

 2015N1013i΁j16F4018F10 v i}gwj uʉ􉽊wɊÂd͗_̍\Ɋւ錤v ʉ􉽊ẃCd͗_̃{\ɂĊ􉽊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邪̔􉽊wIȔzʂɂĂ͈ˑRƂė[܂ ĂƂ͂Ȃ󋵂ɂD @{uł͈ʉ􉽊wɂĐڑƗ]ڑ̖ւuʉ􉽊w̕ώv𓱓邱Ƃɂ􉽊wIȔwi̐VȊ􉽊wỈ\ɂċc_DƂɂ̈ʉ􉽊w̕ώɊÂd͗_̍\ɂĕ񍐂. { 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)

### _wRLEifqj

 2015N929i΁j16F4018F10 iswj uubNz[̃~NȏԂɊւV\ƁAQ[Wd͑Ήւ̉pv ̔wiɑ΂ăJIXIU镑ÓT݂邱ƂmĂB{uł́AŏPoincare' sectionALyapunov spectrumƂJIXt镨ʂЉB̏ŉXNear Penrose limitɂAdS_5~T^{1,1}̃JIXI̐ɂċc_BAdS_5~T^{1,1}ɃJIXI݂邱Ƃ͂łɒmĂ邪AX̌Near Penrose limitɂĂJIXI݂邱Ƃ炩ɂȂBsub-leading correctionݏoZpgbNX\ɂKolmogorov-Arnold-Moser(KAM)g[X󂷂邱ƂɂĂB { wr܃LpX4 ֍u(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^gʂɂĔۓIIɔj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[IȐƂ 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^̑]ڂ݂̂Ƃ̏ؖɗpꂽB̌AAϐixjɑ΂ [__ՊE_ł̃[_̃XP[OȂǂ̗_IgsꂽB ŁA ۂ̃[_̓o͈ʓIɂ͓ۑƂĒmB {uł́AʎqF͊wɂLee-Yang[_藝̉pɂĐBiqQCDɂLee-Yang[_̌vZ@AɂLee-Yang[_͓̉IȂsBQCDLee-Yang[_e[^֐̃[_ƈv邱ƂAiqQCĎvZpĂ̌؂sB܂AߔNsĂ鑊Θ_IdCIՓˎƂ̊֘AȂǂɂĂB { 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

 2015N518ij16F4018F10 O k i{wj u̐Eʂ̔jꂽ[[h1/4BPSEB\[v1/2BPSǏZq̑֊֐ɂāv AdS/CFTΉł̓Q[W_̃EB\[vAdŠ̐Eʂ̑Ή\B܂łEB\[v̊ҒlǏZqƂ̑֊֐ɊւĂ̑Ή֌W؂ĂBł́Ȁꍇ̌ÓTpďd͗_̉͂sB{ł́CɌÓTIȌl̂ł͂ȂA2006NN. Drukkerɂėpꂽgjꂽ[[hhꂽ@c_B܂̉pƂāAEB\[vƋǏZq̑֊֐̌vZЉB { wr܃LpX4 ֍u(4232)

### _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􉽊wIIԂɂĐ 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\@pƁA25wi6̕ɂ֌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֌Wɂċc_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[ɂĒׁA ̉Ae̓𖾂炩ɂB w4 ֍u(4232)

### _wRLEifqj

 2014N1209i΁j16F4018F10 gc Y iswj ud/Yang-BaxterΉɂāv ߔNAAdS5×S5 ̒_̉ϕό舵nIȎ@JꂽB ̎@ɊÂƁA ÓTYang-Baxter𖞂ÓTr-s߂΁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/CFTΉ̉ϕόɊւŋ߂̌ʂɂāA s̃r[ȂЉB ܂AϕAdS5×T{1,1} ̕όւ̉pɂĂB 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񓙕ɂāA ܂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]ׂaɂĘbƎvB w4 ֍u(4232)

### _wRLEiFj

 2014N1010ij16F4018F10 icwj u̒ł̏d͕v ߔNAnti-de-Sitterł̏ď͕ɂA Ԃɂg̃GlM[JXP[hۂ ubNz[ɏdvȖƎwEꂽB ͗ႦΑQߕRȎłIȕߋ@\΋N肤邩B {\ł͂̊̕ȒPȃr[ƂƂɖ𖾂̖ɂċc_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[N߂̑oΒЂƂ͓̉IƂ 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 񎩖ȋƂɋNĂB uł́C߂ɁCNH[N߂Ɋւŋ߂̌̊ȒPȃr[sB ɁCĊ֐肱݌Q̕@pāCSavvidy^Nielsen-Olesens萫 ĂȂȂ邱ƂB ̌_́C(i) ȂLύpC fɒlLύpɑ΂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~~Ղd͉]n̕ՓIȍ\łA ߔN~~Ղێp^ʁEASJjYƂ C]šd̂̃V~[Vɂ萸͓IɂȂĂB AubNz[V̂̍~~Ղł́A dqƃCỈxقȂvY}MIȍGlM[dqϑĂA Փˌnł̍~~Ղ̕dvƂȂĂĂB Z~i[ł́AՓˌn̍~~Ղł̗̍q p^ʗAɂčŋ߂̌ЉB w43K 4340

## 2014Nxtw

### _wRLEiFj

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

### _wRLEifqj

 2014N0708i΁j16F4018F10 Y s icmwj uΏ̊iqQ[W_̐^Ƃ̌Œɂāv 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@ɂĂ̈ʘ_A X@ɂĐB 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) ̑Ώ̐R̋ꗝ_ɗp邱Ƃɂ ۓIɋc_B ΒmM(Kavli IPMU)Ƃ̋ arXiv:1404.0489 ɊÂB w4 ֍u(4232)

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 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[ʁjɂĂc_B w4 ֍u(4232)

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 2014N0527i΁j16F4018F10 ɓ xq iGlM[팤@\j uiqV~[VgConformal windowɊւŋ߂̌ɂāv lQ[W_ɂ 񎩖ȑݍpԊOŒ_݂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)

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 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)

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 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)

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 2014N0428ij16F4018F10 q iwj u뎿ʍKXs܂ފgꂽ̗̏_̍\v {\IJ̏ԋԂne\ς ̏ۂƂɂA ̗̏_뎿ʂɔCӂ̍KXs_ igꂽ̗̏_j ̎Rȍp\ł ƂA̐c_B ̗_́Ȁ̗_Ɠ̃Q[WΏ̐߁A Ώ̐Gȏꍇɂ͈ʂɍł KXsQ[W̃Q[Wsύp̕ՓIȍ\ eՂɂƂ_B ƂāA ̓Iɂ̍KXsQ[W̍p\B ɁAtF~I܂ޏꍇւ̊gA ݍp܂ޗ_ւ̊g\ɂĂc_B w4 ֍u(4232)

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

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 2014N0415i΁j16F4018F10 Ci iwj uJCΏ̐ƕ߁v Schwinger-DysonƓ암-Jona-Lasiniofg JCΏ̐̔jƉ񕜂ɂĂ̊{IȓeƁA NH[N̕߂Ɋ֌WbЉB w4 ֍u(4232)

## 2013Nx Hw

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

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 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)

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 2014N0107i΁j16F4018F10 R Ti iF{wj u[vd͗_̊{ƌv d͂ʎq_IɋLq鎎݂̂PƂāA [vd͗_܂B [vd͗_܂pȂΏۂɁA ̗_Ȃǂ܂ɏЉA ŌɌɂĂȒPɂbł΂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

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 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[Nɂ͕ߗ͂L_قȂB ۓIQCDŃVCK[@\𖾂邽߁A AdS/CFTΉpĒΏQCDŐ^s萫vZB ʂ͕Iɉ߂łẢ܂߂čusB w43K 4340

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 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ɂāA Xs͂̌ʂbƎvD w43K 4340

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 2013N1126i΁j16F4018F10 [J p iwj uAnomaly or symmetry ?v ɂʎqF͊w(QCD)ł́AIɔjĂ SU(2) aJCΏ̐񕜂ƍLMĂ邪A U(1) ̃JCΏ̐ɂĂ ͂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)

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

### _wRLEiFj

 2013N1022i΁j16F4018F10 F_@mI iIPMUj uHigher spin ubNz[Ƃ̃Ggs[ɂāv higher spin _́A XsQȏ̗뎿ʏ(higher spin)܂ޏd͗_łB ߔNAhWb^[ԏhigher spin _ƁA ̋EŒꂽ`̗_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 ̔\ł́ǍʂƁǍ̐iWɂăr[B w4 ֍u(4232)