Spring workshop on gravity and cosmology

Europe/Warsaw
Jagiellonian University

Jagiellonian University

Chunshan Lin, Danilo Artigas (Jagiellonian University) , Jakub Mielczarek (Jagiellonian University) , Jerzy Jurkiewicz (Jagiellonian University)
Description

This is the spring meeting, the continuation of a series of workshops on gravity and cosmology, which was previously held at the University of Warsaw, and has migrated to the Jagiellonian University since this spring.

Due to the pandemic outbreaking, we will have our meeting online on MicroSoft Teams. We focus on the following topics in this meeting: 

(1) theories beyond GR, including classical extension, and quantum gravity; 

(2) gravitational wave probe;

Invited speakers: 

  • Jan Ambjørn (Nijmegen U., IMAPP and Bohr Inst.)
  • Michal Artymowski (Ariel University)
  • Aurelien Barrau (LPSC, Grenoble)
  • Martin Bojowald  (Penn State University)
  • Suddhasattwa Brahma  (McGill University)
  • Yifu Cai (USTC)
  • Giacomo Ciani  (University of Padova & Virgo)
  • Ema Dimastrogiovanni  (New South Wales U.)
  • Matteo Fasiello (ICG, U. Portsmouth)
  • Julien Grain  (Institut d’Astrophysique Spatiale, Orsay)
  • Sachiko Kuroyanagi (Nagoya U., & IFT Madrid)
  • Macarena Lagos (Chicago U., KICP)
  • Antonino Marciano (Fudan University & INFN Frascati Laboratories)
  • Sabino Matarrese (INFN Padova)
  • Shinji Mukohyama (YITP, Kyoto University)
  •  Daniele Oriti (Arnold-Sommerfeld-Center for Theoretical Physics, Munich)
  •  Alejandro Perez (Centre de Physique Théorique, Marseille)
  • Shi Pi (IPMU, Tokyo University)
  • Wlodzimierz ​Piechocki (National Centre for Nuclear Research)
  • Nikodem Poplawski (U. New Haven)
  • Kai Schmitz (CERN)
  • Gianmassimo Tasinato (Swansea University)
  • Yifan Wang (AEI)

How to join us in this meeting?
(1) create a MS account (it is for free);
(2) register our workshop on the indico;
(3) notify me of your MS account.
(4) you will be added into our workshop Teams.
(5) enjoy!


the list of previous workshops, 

2018 winter meeting 

2019 spring meeting

2019 summer Beyond meeting (biannual)

2019 autumn meeting

Registration
spring workshop on gravity and cosmology
Participants
  • Adamantia Zampeli
  • Adithiya Dinesh
  • Adolfo Cisterna
  • Adrià Delhom I Latorre
  • Aichen Li
  • Aim Patel
  • Alejandro Jimenez
  • Aleksandra Nowak
  • Alessandro Camilletti
  • Alessandro Pisana
  • Alessia Platania
  • Alexandra Pi
  • Alvise Raccanelli
  • Ameek Malhotra
  • Ami Patel
  • Andronikos Paliathanasis
  • Andrzej Görlich
  • Anetta Lenar
  • Angelo Ricciardone
  • Anthony Bwembya
  • Antonino Marciano
  • Antonio Pereira
  • Arkadiusz Bochniak
  • Armando A. Roque Estrada
  • Arslan Sikandar
  • Artem Poliszczuk
  • Artur Miroszewski
  • Arvind Kumrar Mishra
  • Athanasios Bakopoulos
  • Aurélien Barrau
  • Avery Hui
  • Aya Iyonaga
  • Babak Beheshti
  • Bartosz Sójka
  • Batool Imtiaz
  • Benedicte Brulin
  • Betti Hartmann
  • Bora Basa
  • Bruno Bucciotti
  • Bruno Sanna
  • Bénédicte Brulin
  • Celia Escamilla-Rivera
  • Chandra Shekhar Saraf
  • Charli Chinmayee Pal
  • chendong sun
  • Cheng Liu
  • Cheng-Jian Luo
  • Chengcheng Han
  • Chiara Animali
  • chonticha Kritpetch
  • Chunshan Lin
  • CRISTHIAN CALDERON
  • Damodar Rajbhandari
  • Daniel Correia
  • Daniel Sobral Blanco
  • Daniela Magos
  • Daniele Bertacca
  • Daniele Oriti
  • Ding Ding
  • Drazen Glavan
  • Dániel Németh
  • Ema Dimastrogiovanni
  • Emine Seyma Kutluk
  • Emir Gumrukcuoglu
  • Etevaldo Costa
  • Fazlu Rahman Panam Parambil
  • Francesca Vidotto
  • François Larrouturou
  • Gabriel Rocha
  • gabriel Unger
  • Gabriel Vidal
  • George Alestas
  • Giacomo Ciani
  • Gianmassimo Tasinato
  • Giovanni Marozzi
  • Giuseppe Clemente
  • GOPAL KASHYAP
  • Gopi Patel
  • Grzegorz Czelusta
  • Guillem Domenech
  • Gustavo Bezerra Silva
  • HARITHA C P
  • Harsha Miriam Reji
  • Hayato Motohashi
  • Heliudson Bernardo
  • Hyat Huang
  • Ibai Asensio Pol
  • Ivonne Zavala
  • Jack Bennett
  • Jackson Levi Said
  • Jakub Bilski
  • Jakub Gizbert-Studnicki
  • James Bonifacio
  • Jan Ambjorn
  • JIANI YE
  • Jie Jiang
  • Jin Qiao
  • Jing Wang
  • Joana Teixeira
  • Jonas Pinheiro da Silva
  • Jose Grimario de Lima Junior
  • Josua Unger
  • Julien Grain
  • Julio Arrechea
  • Jun-Bao Wu
  • Junji Jia
  • Jéferson Fortunato
  • Józef Łapa
  • Júlio Farias
  • Kai Schmitz
  • Karthik Jain
  • Kaye Li
  • Kevin Gonzalez-Quesada
  • Krzysztof Turzyński
  • Kurt Hinterbichler
  • Laura Iacconi
  • Laura Johnson
  • Laurence Bloxham
  • Lauziene Barboza
  • Lavrentios Kazantizidis
  • Leila Graef
  • Lu Yin
  • Lucas Nascimento Monteiro
  • Luiz Filipe Guimarães
  • Macarena Lagos
  • Maciej Kierkla
  • Marcus Reitz
  • Maria Jose Guzman
  • Mark Linton
  • Martin Bojowald
  • Martine Irog
  • Maryam Aghaei Abchouyeh
  • Mateo Pascual
  • Matheus Silva
  • Mathieu Vincensini
  • Matteo Fasiello
  • Matthew Hull
  • Mian Zhu
  • Michael Kenna-Allison
  • Michal Artymowski
  • Michele Oliosi
  • Muhsin Aljaf
  • Nandan Roy
  • Nicola Bartolo
  • Nils A. Nilsson
  • Noureddine Mebarki
  • Obinna Umeh
  • Ogan Ozsoy
  • Omar Alaryani
  • Orest Hrycyna
  • Oto Imrich
  • Parris Trahanas
  • Peng Hui
  • Phongsaphat Rangdee
  • Pierre Martinetti
  • qianhang ding
  • qing lu
  • Rafael Bravo
  • Rafael Robson Lino dos Santos
  • Rahmat Rahmat
  • Raissa Maria Pimentel Neves
  • Rajeev Singh
  • Remigiusz Durka
  • Renata Ferrero
  • Ricardo Escobar
  • Richa Arya
  • Roberto Caroli
  • Roberto Casadio
  • Rogerio Cavalcanti
  • Rogério Augusto Capobianco
  • Ronaldo Paiva
  • Rudnei Ramos
  • Rui Niu
  • Sabino Matarrese
  • Sachiko Kuroyanagi
  • Sagar Kumar Maity
  • SAIKAT CHAKRABORTY
  • Samim Akhtar
  • Santiago Esteban Perez Bergliaffa
  • Sebastian Bahamonde
  • Sebastian Garcia-Saenz
  • Sen Yang
  • Seong Chan Park
  • Sergio Oscar Nuñez Silva
  • Shahab Shahidi
  • Shahab Shahidi
  • Shao-Jiang Wang
  • Shi Pi
  • Shiladitya Porey
  • Shinji Mukohyama
  • SiNan Long
  • Sioree Ansar
  • Snigdha Sharma
  • Sonith LS
  • Sovan Sau
  • Sreejesh Satheesh Kumar
  • Stratos Pateloudis
  • Suddhasattwa Brahma
  • Suman Kumar Panja
  • Sunny Vagnozzi
  • Suphakorn Chunlen
  • Syed Naqvi
  • Taha Malik
  • Tanguy Grall
  • Theodoros Papanikolaou
  • Thomas Colas
  • Tiago Vinicius
  • tigarroumine mohamed
  • Tiziano Schiavone
  • Tomasz Trzesniewski
  • Tristan Madeleine
  • Vahid Kamali
  • Victor I. Afonso
  • Vincent Vennin
  • Vishnu Rajagopal
  • Vladimir Pastushenko
  • Vladimir Soloviev
  • wei fang
  • Weslley Barros
  • William Wolf
  • Włodzimierz Piechocki
  • Xi Tong
  • Xinhe Meng
  • xinrui wei
  • Xu Na
  • Xun Xue
  • Yasmine Mhirsi
  • Yasser Elmahalawy
  • Yi Wang
  • Yi-Fu Cai
  • Yifan Wang
  • Yifei Li
  • Yili Wang
  • Yingli Zhang
  • yipeng liu
  • Yong Cai
  • Yong Tang
  • Yoxara S. Villamizar
  • Yuan He
  • Yuanzhang Cui
  • Yuhang Zhu
  • Yumeng Xu
  • Yun Fang
  • Yun-Long Zhang
  • Zbigniew Drogosz
  • Zhiqi Huang
  • 乾 (qian) 向
  • 祁 李
    • 09:55 17:50
      session I
      • 10:00
        reception 25m
      • 10:25
        The (glorious) past, (exciting) present and (foreseeable) future of gravitational wave detectors. 50m

        The first trace left by a gravitational wave in a man-made detector in September 2015 marked the birth of gravitational wave astronomy. Less than four years from that first signal, gravitational wave detections have become routine, the LIGO and VIRGO instruments are standing up to their mission of being "observatories" and the trove of signals collected is enabling exciting new science and multi-messenger astronomy. And yet, the gravitational wave community has plans to expand the band, reach and sensitivity of detectors even further.
        I will quickly review the experimental basis of gravitational wave detection, the status of the current detectors with highlight on the most significant detections performed so far, and try to shed some light on what's coming next.

        Speaker: Giacomo Ciani
      • 11:15
        coffee break 30m
      • 11:45
        Probing the Physics of the Early Universe with Gravitational Wave Experiments 50m
        Speaker: Gianmassimo Tasinato
      • 12:35
        Gravitational-Wave Implications for the Parity Symmetry of Gravity at GeV Scale 25m
        Speaker: Yifan Wang
      • 13:00
        lunch break 1h
      • 14:00
        some new results on quasinormal modes of black holes 50m

        I will show how quasinormal modes of black holes can be used to investigate new physics and quantum gravity. Some results on isospectrality will also be underlined.

        Speaker: Aurélien Barrau
      • 14:50
        Theory confronts Observations: Cosmology in the era of the Swampland 25m

        It is well-known that accelerating spacetimes form the basis of our understanding of early and late-time cosmology. On the other hand, there has been a pile of mounting evidence, mainly based on numerous results from String Theory (but not limited to them), that de Sitter space is difficult to embed in a quantum theory of gravity. Thus, these theoretical constraints that any consistent effective field theory must satisfy in order to have a UV-completion -- the so-called "Swampland conjectures" -- form a new challenge for phenomenologically viable model-building in cosmology. In this talk, I shall discuss some aspects of these conjectures, evidence in support of them and how to reconcile them with astronomical observations with a special focus on inflation. The importance of non-perturbative quantum corrections in constructing quasi de-Sitter backgrounds shall also be demonstrated.

        Speaker: Suddhasattwa Brahma
      • 15:15
        coffee break 30m
      • 15:45
        Physical implications of a fundamental period of time 50m
        Speaker: Martin Bojowald
      • 16:35
        Quantum fluctuations of the compact phase space cosmology 25m

        In the recent article Phys. Rev. D 100, no. 4, 043533 (2019) a compact phase space generalization of
        the flat de Sitter cosmology has been proposed. The main advantages of the compactification is that
        physical quantities are bounded, and the quantum theory is characterized by finite dimensional Hilbert
        space. The purpose of this presentation is to discuss the extraction of semiclassical effects from this
        model by way of canonical effective methods. First, a brief review of canonical effective methods is
        given. Afterwards, we discuss the character of the semiclassical solutions of the compact phase space
        cosmological model. Finally, a relation between the behavior of the quantum fluctuations of the
        cosmological sector and the holographic Bousso bound is discussed.

        Speaker: Sean Crowe
    • 10:00 19:05
      session II
      • 10:00
        A consistent theory of D -> 4 Einstein-Gauss-Bonnet gravity 50m

        TBA

        Speaker: Prof. Shinji Mukohyama (YITP, Kyoto University)
      • 10:50
        Quantum Ostrogradsky theorem 25m
        Speaker: Hayato Motohashi
      • 11:15
        coffee break 30m
      • 11:45
        Gravitational Waves from Cosmological B-L Breaking 50m

        The type-I seesaw mechanism crucially depends on the presence of right-handed neutrinos (RHNs) with large Majorana masses. These heavy RHN neutrinos are, however, notoriously hard to produce in terrestrial experiments, which impedes their experimental discovery. In the present talk, I will therefore present a novel, cosmological window onto the seesaw mechanism: the gravitational-wave (GW) signal associated with the cosmological phase transition in the early Universe during which RHNs acquire their mass. I will discuss both first-order and second-order phase transitions as well as GW production from both bubble collisions and cosmic strings. As I will show, the expected GW signal is going to be within the reach of upcoming GW experiments in large parts of the seesaw parameter space, opening up the possibility to probe a variety of RHN and leptogenesis scenarios in the near future. This talk is based on work in collaboration with Simone Blasi, Vedran Brdar, Wilfried Buchmuller, Valerie Domcke, Kohei Kamada, and Hitoshi Murayama (see 1305.3392, 1912.03695, 2004.02889).

        Speaker: Kai Schmitz
      • 12:35
        Ongoing Efforts to Constrain Lorentz Symmetry Violation in Gravity 25m
        Speaker: Nils A. Nilsson
      • 13:00
        lunch break 1h
      • 14:00
        CDT, a theory of quantum geometry. 50m

        Causal Dynamical Triangulations (CDT) is a lattice model which provides a non-perturbative, background independent formulation of four-dimensional quantum gravity. It provides an emergent background geometry and one can study the quantum fluctuations around this background geometry. The model has second order phase transition lines in the bare coupling constants. These transition lines may be used to test the asymptotic safety scenario of quantum gravity. A minisuperspace effective action can be reconstructed from the data obtained from computer simulations of the model. By studying geometries where the spatial topology is toroidal we can "reintroduce" coordinates and attempt to construct a complete effective action.

        Speaker: Prof. Jan Ambjørn (Bohr Ins.)
      • 14:50
        Loop-based observables in 4D CDT 25m
        Speaker: Zbigniew Drogosz
      • 15:15
        coffee break 30m
      • 15:45
        Cosmic Fibers and the parametrization of time in CDT quantum gravity 25m
        Speaker: Daniel Németh
      • 16:10
        Spectral Analysis of Causal Dynamical Triangulations via Finite Element Methods 25m

        I will describe the current state of research on the application of spectral methods to the
        Quantum Gravity approach known as Causal Dynamical Triangulations (CDT).
        Firstly, I will give an overview of the class of analysis methods based on graph theory
        applied to the dual graphs of simplicial manifolds, arguing why they are inadequate, in some regimes,
        to capture distance information, therefore distorting some of the current results (e.g., the dimensional reduction plot).
        Secondly, I will present a method based on finite elements as solution to this problem, showing
        a toy model where the previous method blatantly fails and some preliminary results on its application to
        CDT configurations.

        Speaker: Giuseppe Clemente
      • 16:35
        4-D Gauss Bonnet from an Amplitudes Perspective 25m
        Speaker: Laura Johnson
    • 10:00 17:50
      session III
      • 10:00
        Looking for a healthy nonsingular bounce 50m

        In this talk I plan to review the cosmological paradigm of nonsingular bounces, which is often regarded as an alternative to inflation in describing the very early universe. Such a scenario, while can avoid the big bang spacetime singularity, often suffers from conceptual challenges, namely, the dangerous growth of anisotropic stress, the possibly existence of ghosts, gradient instabilities or even superluminal propagation of primordial perturbations. I will introduce how these issues can be addressed in turn, which push the study on nonsingular bounce towards a possibly healthy version. Recently, a novel nonsingular bounce model was proposed based on the most generic scalar tensor theory dubbed the DHOST theory, which can mostly resolve the aforementioned conceptual challenges within a covariant form. This new cosmology shall inspire a series of follow-up studies from theoretical, phenomenological and observational perspectives.

        Speaker: Prof. Yifu Cai (University of Science and Technology of China)
      • 10:50
        Stable Cosmology in Generalised Massive Gravity 25m
        Speaker: Michael Kenna-Allis
      • 11:15
        coffee break 30m
      • 11:45
        Gravitational footprints of massive neutrinos and lepton number breaking 50m

        We investigate the production of primordial Gravitational Waves (GWs)
        arising from First Order Phase Transitions (FOPTs) associated to
        neutrino mass generation in the context of type-I seesaw schemes. We
        examine both “high-scale” as well as “low-scale” variants, with either
        explicit or spontaneously broken lepton number symmetry. In the latter
        case, a pseudo-Goldstone boson, dubbed majoron, may provide a
        candidate for warm or cold cosmological dark matter. We find that
        schemes without majoron lead to either no FOPTs or too weak FOPTs,
        precluding the detectability of GWs in present or near future
        experiments. Nevertheless, we found that, in the presence of majorons,
        one can have strong FOPTs and non-trivial primordial GW spectra which
        can fall well within the frequency and amplitude sensitivity of
        upcoming experiments, including LISA, BBO and u-DECIGO. We further
        analyze the associated types of FOPTs and show that in certain cases,
        the resulting GW spectra entail, as characteristic features, double or
        multiple peaks, which can be resolved in forthcoming experiments. We
        also found that the majoron variant of the low-scale seesaw mechanism
        implies a different GW spectrum than the one expected in the
        high-scale majoron seesaw. This feature will be testable in future
        experiments. Our analysis shows that GWs can provide a new and
        complementary portal to test the neutrino mass sector.

        Speaker: Antonino Marciano
      • 12:35
        Cosmology with unparticles: Bounces, inflation, cyclic Universe and dark energy 25m

        Our understanding of the Universe is based on general relativity and on the standard model of fundamental interactions. This picture suffers from several issues that cannot be explained by GR or SM, like primordial singularity, inflation, dark energy or dark matter. I will show how unparticles may solve at least some these problems and generate realistic cyclic Universe and dark energy

        Speaker: Michal Artymowski
      • 13:00
        lunch break 1h
      • 14:00
        Some aspects of stochastic background of gravitational waves 50m

        Our universe is fulfilled by stochastic background of gravitational waves with a large range of frequencies, which may have various astrophysical/cosmological origins in the early universe. As our universe is transparent to gravitational wave, it is a fossil recording the information of its generation and how our universe evolves. In this talk I will briefly review the stochastic background of the gravitational waves, especially the secondary gravitational waves induced by scalar perturbations and their connection to the primordial black holes as dark matter. I will also introduce our recent work on the shapes of the spectrum: infrared scaling and the peak.

        Speaker: Dr Shi Pi (IPMU, Tokyo University)
      • 14:50
        Induced gravitational waves in general cosmologies 25m

        Gravitational waves (GWs) are unavoidably induced at second order in cosmological perturbation theory. The so-called induced GWs are a crucial counterpart of the primordial black hole scenario and might be observable by future space based gravitational waves detectors. However, only the generation during radiation and matter domination eras has been analytically studied. In this talk, I will show new analytical results for the scalar induced GWs in decelerating cosmologies. I will argue that the induced GW spectrum can be a probe of the thermal history of the universe. Lastly, I will discuss possible degeneracies with known sources, such as first order phase transitions.

        Speaker: Dr Guillem Domenech (Heidelberg university)
      • 15:15
        coffee break 30m
      • 15:45
        Big Bounce and inflation from spin and torsion 50m

        The conservation law for the total (orbital plus spin) angular momentum of a Dirac particle in the presence of gravity requires that spacetime is not only curved, but also has a nonzero torsion.
        The coupling between the spin and torsion in the Einstein-Cartan theory of gravity generates gravitational repulsion at extremely high densities, which should prevent a singularity in a black hole and may create there a new, closed, baby universe.​
        We show that such a universe may form when a particular function of the scale factor and temperature is greater than some threshold, and that the universe can undergo one or more nonsingular bounces.​
        We also show that quantum particle production caused by an extremely high curvature near a bounce, and creating enormous amounts of matter, can generate a finite period of inflation.​
        This scenario has only one parameter, does not depend significantly on the initial conditions, does not involve hypothetical scalar fields, avoids eternal inflation, and predicts plateau-like inflation that is supported by the Planck observations of the cosmic microwave background.​
        This scenario also suggests that our Universe may have originated from a nonsingular Big Bounce in a black hole existing in another universe.

        Speaker: Nikodem Poplawski
      • 16:35
        Proof of the quantum null energy condition for free fermionic field theories 25m
        Speaker: Taha Malik
    • 10:00 18:15
      session IV
      • 10:00
        Testing Inflation with Primordial Messengers 35m
        Speaker: Mr Matteo Fasiello (ICG)
      • 10:35
        Gravitational waves from inflation 40m
        Speaker: Ms Ema Dimastrogiovanni (New South Wales U)
      • 11:15
        coffee break 30m
      • 11:45
        Searching for gravitational wave bursts from cosmic string cusps with the Parkes Pulsar Timing Array 50m

        Cosmic strings are one of the gravitational wave (GW) sources that can be probed by pulsar timing arrays (PTAs). In this work we develop a detection algorithm for the GW burst from a cusp on a cosmic string, and apply it to a Parkes PTA data release. We find four events with a false alarm probability less than 1\%. However further investigation shows that all of these are likely to be spurious. As there are no convincing detections we place upper limits on the GW amplitude for different event durations. From these bounds, we place limits on the cosmic string tension, that are independent from other bounding techniques. Finally, we discuss the physical implications of our results and the prospect of probing cosmic strings in the era of Square Kilometre Array.

        Speaker: Sachiko Kuroyanagi
      • 12:35
        Gravitational Waves from a Rolling Axion Monodromy 25m

        In string theory inspired models of axion-like fields, sub-leading non-perturbative effects, if sufficiently large, can introduce steep cliffs and gentle plateaus onto the underlying scalar potential. During inflation, the motion of a spectator axion in this potential becomes temporarily fast, leading to exponential amplification of one helicity state of gauge fields. In this model, the axion- gauge field sector interacts gravitationally with the inflaton, therefore the resulting sourced scalar and tensor fluctuations are produced only through gravitational interactions. Due to the tem- porary speeding up of σ in the cliff-like regions, the tensor and scalar correlators sourced by the gauge fields exhibit a localized bump in momentum space corresponding to the modes that exit the horizon while the roll of σ is significant. Thanks to the gravitational coupling of gauge fields with the visible sector and the localized nature of particle production, this model can generate observable gravitational wave signal at CMB scales while satisfying the current limits on scalar perturbations. The resulting gravitational wave signal breaks parity and exhibit sizeable tensor non-Gaussianity that can be probed by future CMB B-mode missions. Depending on the initial conditions on σ and model parameters, the roll of the spectator axion can also generate an ob- servably large GW signature at interferometer scales while respecting the bounds on the scalar fluctuations from primordial black hole limits.

        Speaker: Ogan Ozsoy
      • 13:00
        lunch break 1h
      • 14:00
        Anisotropies and non-Gaussianity in Cosmic Microwave and Gravitational-Wave Backgrounds 50m
        Speaker: Sabino Matarrese
      • 14:50
        Constraining the inflationary field content 25m
        Speaker: Laura Iacconi
      • 15:15
        coffee break 30m
      • 15:45
        Testing Cosmology with Gravitational Waves 50m

        As we enter the era of precision cosmology, the behavior of gravity on large scales and the nature of the main constituents of the universe still remain debatable. Future data from the Cosmic Microwave Background and galaxy surveys, along with the advent of gravitational waves (GW) will provide us precise constraints that will help uncover some cosmological puzzles.
        In this talk, I will focus on testing the nature of dark energy with GW. I will show how we can generically study possible modifications to the concordance LCDM model in a unified manner, and discuss how GW are affected. Then, I will show how these modifications can be constrained with observations of binary neutron stars and discuss results for LIGO.

        Speaker: Macarena Lagos
      • 16:35
        Probing Gravitational Couplings in Dark Energy Theories 25m
        Speaker: William Wolf
    • 09:05 17:25
      session V
      • 10:00
        The universe as a quantum gravity condensate and effective cosmological dynamics 50m
        Speaker: Daniele Oriti
      • 10:50
        Approximate Killing symmetries in non-perturbative quantum gravity 25m
        Speaker: Marcus Reitz
      • 11:15
        TBA 30m
      • 11:45
        Possible observational consequences of Planckian granularity 50m

        I will argue that discreteness at the Planck scale (naturally expected to arise from quantum gravity) might manifest in the form of minute violations of energy-momentum conservation of the matter degrees of freedom when described in terms of (idealized) smooth fields on a smooth spacetime. In the context of applications to cosmology, such “energy diffusion” from the low energy matter degrees of freedom to the discrete structures underlying spacetime would lead to the emergence of an effective dark energy term in Einstein’s equations. We estimate this effect using a (relational) hypothesis about the materialization of discreteness in quantum gravity which is motivated by the strict observational constraints supporting the validity of Lorentz invariance at low energies. Arguments based on a simple dimensional analysis lead to an estimate of an effective cosmological constant agreeing in order of magnitude with its observed value. I will also mention possible implications in the more recent dynamics of the universe.

        Speaker: Alejandro Perez
      • 12:35
        Disformal transformations in modified teleparallelism 25m
        Speaker: Maria Jose Guzman
      • 13:00
        lunch break 1h
      • 14:00
        Quantum fate of the BKL scenario 50m

        I will present the quantum model of the asymptotic dynamics underlying the Belinski-Khalatnikov-Lifshitz (BKL) scenario. The classical BKL scenario concerns generic singularity of general relativity. The quantum BKL scenario shows that gravitational singularity can be replaced by quantum bounce. I will suggest that quantum general relativity has a good chance to be free from singularities.

        Speaker: Włodzimierz Piechocki
      • 14:50
        coffee break 30m
      • 15:20
        Stochastic shear in bouncing cosmologies 50m

        Bouncing cosmologies is a popular alternative to (or an extension of) primordial inflation. However, the contracting phase preceding the bounce is known to be flawed with a shear instability with important consequences on the fate of the bouncing universe. Depending on the concrete model, this instability could either prevent the bounce to occur or drive the universe in an expanding phase radically different from the observed one. I will show that even in the absence of initial shear, quantum fluctuations of the matter content lead to a non-zero anisotropic stress. This unavoidable anisotropic stress is stochastic by nature and sources a non-zero shear. The amount of stochastic shear built up by quantum fluctuations is computed considering the simple situation of a massless scalar field and using the stochastic « inflation » formalism to describe its quantum fluctuations. I’ll show that for a soft equation-of-state, i.e. w>-1/9, the shear contribution remains small enough up to the bounce and there is no additional source of shear instability. However, for w<-1/9, the shear backreaction becomes non-negligible because quantum fluctuations in that case have a spectrum which is too red.

        Speaker: Julien Grain