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Lecture room A, Ground floorSpecial SeminarConference Hall, Farmanieh Building (1st floor)Special SeminarFarmanieh Seminar RoomSpecial SeminarFarmanieh Seminar RoomString Theory Group MeetingString Theory Group Meeting Farmanieh Seminar Room String Theory Group MeetingFarmanieh Seminar Room String Theory Group MeetingFarmanieh Seminar RoomString Theory Group MeetingFarmanieh Seminar Room Canceled From:   JanFebMarAprMayJunJulAugSepOctNovDec12345678910111213141516171819202122232425262728293031 19901991199219931994199519961997199819992000200120022003200420052006200720082009201020112012201320142015201620172018201920202021202220232024 To:   JanFebMarAprMayJunJulAugSepOctNovDec12345678910111213141516171819202122232425262728293031 19901991199219931994199519961997199819992000200120022003200420052006200720082009201020112012201320142015201620172018201920202021202220232024
 Tue Jan 24, 2023 (1401/11/4) Jan 241401/11/4 14:00 On the Merger Rate of Primordial Black Holes in Cosmic Voids Show Abstract Abstract:Cosmic voids are known as underdense substructures of the cosmic web that cover a large volume of the Universe. It is known that cosmic voids contain a small number of dark matter halos. Regarding this, the existence of primordial black holes (PBHs) in these secluded regions of the Universe is not unlikely. In this talk, I intend to speak about our recent analysis on the merger rate of PBHsin cosmic voids and their contribution to gravitational wave events resulting from black hole mergers recorded by the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO)-Advanced Virgo (aVirgo) detectors. Lecturer(s): Saeed Fakhry From : K.N. Toosi University of Technology Research Group: HEPCO Group Weekly Seminar More Info. : link Tue Jan 17, 2023 (1401/10/27) Jan 171401/10/27 14:00 Temporal vs Spatial Conservation and Memory Effect in Electrodynamics Show Abstract Abstract:We consider the standard Maxwell's theory in 1+3 dimensions in the presence of a timelike boundary. In this context, we show that (generalized) Ampere-Maxwell's law appears as a Noether charge associated with the Maxwell U(1) gauge symmetry which satisfies a spatial conservation equation. Furthermore, we also introduce the notion of spatial memory field and its corresponding memory effect. Finally, similar to the temporal case through the lens of Strominger's triangle proposal, we show how spatial memory and conservation are related. Lecturer(s): Mohammad Hasan Vahidinia From : Institute for Advanced Studies in Basic Sciences (IASBS) Research Group: HEPCO Group Weekly Seminar More Info. : link Tue Jan 10, 2023 (1401/10/20) Jan 101401/10/20 14:00 On the detection statistics in a double-double-slit experiment Show Abstract Abstract:Double-slit experiment has always been one of the central experiments in quantum mechanics. Yet, if there is an experiment more mysterious, it is a double-double-slit experiment with entangled particle pairs. In this experiment, the two most important properties of quantum theory, i.e. superposition and entanglement, combine and lead to a non-local interference pattern. The full analysis of this experiment can be even more complex because of the third quantum effect, i.e. the collapse of the wave function when the first particle is detected in the middle of the experiment at random times. This, in principle, can change the detection statistics of the remaining particle. The analysis however is not completely straightforward in standard formalism. One of the reasons is that in the orthodox quantum mechanics we do not have a clear and agreed prediction of detection times distribution. This problem is actually very old, but it is still open. The mathematical origin of this problem is that the time is a parameter in the standard formalism, not a self-adjoint operator, hence, there is no unique and unambiguous way to compute the temporal probability distribution of detection events. Therefore, it is even not clear how one can determine the state of the system at a given time from initial two particle state; because the state and its equation of motion change at an undetermined time. In this talk, we investigate this experiment via Bohmian mechanics which can circumvent this problem and leads to a clear prediction in this situation. Lecturer(s): Mohammad Javad Kazemi From : Sharif University of Technology Research Group: HEPCO Group Weekly Seminar More Info. : link Tue Jan 03, 2023 (1401/10/13) Jan 031401/10/13 14:00 Constraints from the duration of supernova neutrino burst on resonant light gauge boson production by neutrinos Show Abstract Abstract:We discuss the resonant production of low-mass vector mediators from neutrino antineutrino interactions in the core of proto-neutron stars, and determine how they may affect the neutrino energy distribution and their diffusion time in the first seconds after the supernova explosion. Taking into account the radial dependence of the density, energy, and temperature inside the proto-neutron star, we determine the neutrino-antineutrino interaction rate in the star interior in two well-motivated new physics scenarios that feature a low-mass vector mediator, namely $U(1)_{Bâ??L}$ and $U(1)_{ L_\mu â??L_\tau}$ . First, we determine the values of the coupling above which the neutrino self-interaction dominates over the standard neutrino nucleon scattering. We argue that, although in this regime a redistribution of the neutrino energies might take place, this only affects a small part of the neutrino population and cannot be constrained with the SN 1987A data. Thus, contrary to previous claims, the region of the parameter space where this model explains the discrepancy in the muon anomalous magnetic moment is not ruled out. We then focus on small gauge couplings, for which the decay length of the new gauge boson is comparable to (or larger than) the size of protoneutron star. We show that in this regime, the duration of the neutrino burst can be significantly reduced, and values of the coupling as small as O($10^{â??9}$) can be probed, ruling out new areas of the parameter space. These results are relevant for any other model that features new MeV-scale mediators that couple to the neutrino sector. Lecturer(s): Yasaman Farzan From : School of Physics, IPM Research Group: HEPCO Group Weekly Seminar More Info. : link Tue Oct 04, 2022 (1401/7/12) Oct 041401/7/12 14:00 The effect of the interaction of dark matter and dark energy in galactic physics and the ISW effect Show Abstract Abstract:Since most of the matter (energy) of the universe consists of dark matter and dark energy, it is not unlikely that there is even a weak interaction between the dark elements. In this presentation, we draw on the results of two previously performed simulations of cluster-sized haloes with self-interacting dark matter and present previous work on the density profile of galaxy clusters. describe completely. This density profile helps to find a velocity dispersion profile and the relation between cluster mass and density center. We consider two uses of galaxy clusters with these relations: the mass velocity dispersion and temperature relation. We also discuss the effect of this interaction on the profile of the mass function in the galactic halo and the ISW effect. Lecturer(s): Javad Taghizadeh Firouzjaee From : K.N. Toosi University of Technology Research Group: HEPCO Group Weekly Seminar More Info. : link Tue Sep 20, 2022 (1401/6/29) Sep 201401/6/29 14:00 Boundary Conditions of Warped AdS_3 in GMG Show Abstract Abstract:In this talk, in the framework of general massive gravity, I am looking at the asymptotic symmetry, the solution space, and the global charges using the ACDS boundary conditions in the quadratic ensemble. We also show that the boundary counting of the degeneracy of states correctly reproduces the bulk thermodynamic entropy for WBTZ black holes. Lecturer(s): Seyed Naseh Sajadi From : School of Physics, IPM Research Group: HEPCO Group Weekly Seminar More Info. : link Wed Apr 06, 2022 (1401/1/17) Apr 061401/1/17 18:00 Uncovering Energetic Processes in the Interstellar/Intergalactic Medium with the Square Kilometre Array Show Abstract Abstract:Investigating the physics and energetic of the medium where galactic structures, on various scales, are formed is the most fundamental step to understand the formation and evolution of galaxies. Modern galaxy evolution models suggest gas accretion from the intergalactic medium (IGM) or from cosmic filaments as a mechanism to maintain star formation and active galactic nucleus (AGN). Through gas heating and/or gas removal, these models also propose supernova feedback and AGN feedback as mechanisms to quench massive star formation. Observational studies, however, have not reached to a conclusive result showing that feedback can, in some cases, trigger star formation, leaving the issue as an open challenge. It seems that some basic concepts about the formation of structures in the interstellar medium (ISM) and the IGM are missed: What are physical parameters/agents governing the structure formation on various scales? How does the ISM/IGM energy balance change over cosmic time? The advent of the square kilometre array (SKA) and its instrumental capabilities tracing the most energetic ISM components has opened a new window shedding light on the issue. The SKA's sensitive radio continuum observations will trace high-energy particles and magnetic fields not only in star forming regions and AGNs, but also in more quiescent regions in molecular clouds and diffuse IGM, enabling us to study the role of magnetic fields/cosmic rays in structure formation. Sensitive radio continuum observations on large scales may also bring constrains on the entity of dark matter mapped by the Hubble Space Telescope (HST) and Dark Energy Camera (DECam). Lecturer(s): Fatemeh Tabatabaei From : IPM, School of Astronomy Research Group: Physics Colloquium More Info. : Link Tue Mar 15, 2022 (1400/12/24) Mar 151400/12/24 14:00 Amazing Neutrino Particles Lecturer(s): Yasaman Farzan From : School of Physics Research Group: HEPCO Group Weekly Seminar More Info. : link Tue Mar 08, 2022 (1400/12/17) Mar 081400/12/17 14:00 Stochastic Effects in inflationary cosmology Show Abstract Abstract:In this talk, I will speak about the stochastic effects in inflationary cosmology. To this end firstly I will review the stochastic formalism and discuss the properties of the Wiener process in general. In the second part, I will review how the stochastic effects can emerge in inflationary cosmology and why studying these effects in the early universe cosmology is important. Finally, the applications of these effects in different models are discussed. In particular, I will speak about the stochastic effects in axion inflation and the formation of primordial black holes. Lecturer(s): Amin Nassiri Raad From : School of Astronomy, IPM Research Group: HEPCO Group Weekly Seminar More Info. : Link Wed Mar 02, 2022 (1400/12/11) Mar 021400/12/11 18:00 Dance of Cause and Effect: Fluctuation Induced Reduction of Dissipation in Classical Fluids Show Abstract Abstract:About seventy years ago, G I Taylor noticed that the tails of two closely swimming spermatozoa, oscillate in a synchronized fashion as if both of them are controlled from one regulating center. The two sperms, on the other hand, has no mean of communication, but the viscous fluid in which they are swimming. To address the why question, behind the observation, he suggested the minimization of total dissipation in the viscous medium. Sixty years later, Taylors original idea was put to more detailed analytical investigations; non-intuitively, it failed to attribute the observed synchronization to the expected reduction of dissipation. We begin with a very different problem: (a) The motion of two passively trapped beads, which interact through hydrodynamic interactions, and face a driven flow. Both theoretically and experimentally we observe that they almost follow the very motion they would have, if they were to swim on their own in the opposite direction of the driven flow. Calling the phenomenon, the reverse dance, we successfully attribute it to the reduction of the total dissipation. We then (b) extend the minimalistic approach, to two sets of beads; each supposed to mimic the tail of one spermatozoon. Facing a driven flow, on top of their intrinsic oscillation, this is a minimalistic model to verify Taylors idea. The question is, does this simple model lead us to synchronization as well as reduction of fluids dissipation? And if so, can it explain why Taylors original model failed to correctly attribute synchronization with reduction of dissipation? Lecturer(s): Seyyed Nader Rasuli From : University of Guilan & School of Physics, IPM Research Group: Physics Colloquium More Info. : Link *** Please Search (Top of the page) to see more seminars. ***

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