TeVPA08 Beijing -24 September 2008 1 Space-time defects and the accelerated expansion of the universe: an alternative to dark energy? Angelo Tartaglia.

Slides:



Advertisements
Similar presentations
An elastic Lagrangian for space-time
Advertisements

Dr Martin Hendry University of Glasgow. Why are we here?…. The period of inflation in the very early Universe was invoked to explain some apparent fine.
Theories of gravity in 5D brane-world scenarios
Hot topics in Modern Cosmology Cargèse - 10 Mai 2011.
Rainbow Gravity and the Very Early Universe Yi Ling Center for Gravity and Relativistic Astrophysics Nanchang University, China Nov. 4, Workshop.
The Fate of the Universe. The cosmological principle The simplest universes is: Homogenous – the same everywhere you go Isotropic – the same in all directions.
Extragalactic Astronomy & Cosmology First-Half Review [4246] Physics 316.
Yashar Akrami Modern Cosmology: Early Universe, CMB and LSS/ Benasque/ August 17, 2012 Postdoctoral Fellow Institute of Theoretical Astrophysics University.
Exact string backgrounds from boundary data Marios Petropoulos CPHT - Ecole Polytechnique Based on works with K. Sfetsos.
Observational Constraints on Sudden Future Singularity Models Hoda Ghodsi – Supervisor: Dr Martin Hendry Glasgow University, UK Grassmannian Conference.
May 28, 2010, Dezhou A Realistic Torsion Cosmological Model Li Xin-Zhou Shanghai United Center for Astrophysics, Shanghai Normal University.
Cosimo Stornaiolo INFN-Sezione di Napoli MG 12 Paris July 2009.
E. Rakhmetov, S. Keyzerov SINP MSU, Moscow QFTHEP 2011, September, Luchezarny, Russia.
PRESENTATION TOPIC  DARK MATTER &DARK ENERGY.  We know about only normal matter which is only 5% of the composition of universe and the rest is  DARK.
Tomographic approach to Quantum Cosmology Cosimo Stornaiolo INFN – Sezione di Napoli Fourth Meeting on Constrained Dynamics and Quantum Gravity Cala Gonone.
Physics 133: Extragalactic Astronomy ad Cosmology Lecture 5; January
Dark energy and dust matter phases form an exact f(R)-cosmology model Prado Martín Moruno IFF (CSIC) ERE2008 S. Capozziello, P. Martín-Moruno and C. Rubano.
Cosmology Overview David Spergel. Lecture Outline  THEME: Observations suggest that the simplest cosmological model, a homogenuous flat universe describes.
The Ideas of Unified Theories of Physics Tareq Ahmed Mokhiemer PHYS441 Student.
Physics 133: Extragalactic Astronomy ad Cosmology Lecture 4; January
Final Parametric Solution. A Quick Overview of Relativity Special Relativity: –The manifestation of requiring the speed of light to be invariant in all.
1 L. Perivolaropoulos Department of Physics University of Ioannina Open page
Cosmological Models II Connecting Hubble’s law and the cosmological scale factor What determines the kind of Universe in which we live? The Friedman equation.
Galaxies and Cosmology 5 points, vt-2007 Teacher: Göran Östlin Lecture 6.
Lecture 21 Cosmological Models ASTR 340 Fall 2006 Dennis Papadopoulos.
Based on Phys.Rev.D84:043515,2011,arXiv: &JCAP01(2012)016 Phys.Rev.D84:043515,2011,arXiv: &JCAP01(2012)016.
18 September 2001Astronomy 102, Fall Einstein at Caltech, 1933 Today in Astronomy 102: relativity In the next five lectures we will discuss Einstein’s.
HOLOGRAPHY, DIFFEOMORHISMS, AND THE CMB Finn Larsen University of Michigan Quantum Black Holes at OSU Ohio Center for Theoretical Science September
GENERAL PRINCIPLES OF BRANE KINEMATICS AND DYNAMICS Introduction Strings, branes, geometric principle, background independence Brane space M (brane kinematics)
Effective field theory approach to modified gravity with applications to inflation and dark energy Shinji Tsujikawa Hot Topics in General Relativity And.
Chaplygin gas in decelerating DGP gravity Matts Roos University of Helsinki Department of Physics and and Department of Astronomy 43rd Rencontres de Moriond,
Emergent Universe Scenario
The Theory/Observation connection lecture 1 the standard model Will Percival The University of Portsmouth.
Cosmology, Inflation & Compact Extra Dimensions Chad A. Middleton Mesa State College March 1, 2007 Keith Andrew and Brett Bolen, Western Kentucky University.
Dark Energy & High-Energy Physics Jérôme Martin Institut d’Astrophysique de Paris.
Announcements The final exam will be at Noon on Monday, December 13 in Van Allen Hall LR1. The final exam will be cumulative. The final will be 40 questions,
Expansion of the Universe Natural consequence of the basic field equations of the General Theory of Relativity (GTR) When GTR was first developed in the.
Fundamental Principles of General Relativity  general principle: laws of physics must be the same for all observers (accelerated or not)  general covariance:
The Fate of the Universe
Higher Order Curvature Gravity in Finsler Geometry N.Mebarki and M.Boudjaada Département de Physique Mathématique et Subatomique Faculty of Science, Mentouri.
Dark Energy. Expanding Universe Galaxies in the universe are spreading out over time. –Hubble’s law From Einstein’s general relativity this happens as.
The Strained State Cosmology Angelo Tartaglia Politecnico di Torino and INFN.
General Relativity Physics Honours 2009
IX ème Ecole de Cosmologie, Cargese, November 3, Structure formation as an alternative to dark energy Syksy Räsänen University of Geneva Syksy.
A Metric Theory of Gravity with Torsion in Extra-dimension Kameshwar C. Wali (Syracuse University) Miami 2013 [Co-authors: Shankar K. Karthik and Anand.
General Relativity Physics Honours 2008 A/Prof. Geraint F. Lewis Rm 560, A29 Lecture Notes 10.
Anisotropic Evolution of D-Dimensional FRW Spacetime
Influence of dark energy on gravitational lensing Kabita Sarkar 1, Arunava Bhadra 2 1 Salesian College, Siliguri Campus, India High Energy Cosmic.
Cosmic Inhomogeneities and Accelerating Expansion Ho Le Tuan Anh National University of Singapore PAQFT Nov 2008.
The Theory of Special Relativity. Learning Objectives  Einstein’s two postulates in his theory of special relativity: The principle of relativity. (Same.
Inflationary Theory of Primordial Cosmological Perturbation Project for General Relativity (Instructor: Prof.Whiting) Sohyun Park.
General Relativity Physics Honours 2008 A/Prof. Geraint F. Lewis Rm 560, A29 Lecture Notes 9.
Astro-2: History of the Universe Lecture 10; May
ERE 2008September 15-19, Spanish Relativity Meeting 2008, Salamanca, September (2008) Avoiding the DARK ENERGY coincidence problem with a COSMIC.
5th Italian-Sino Workshop on Relativistic Astrophysics Taipei - Hualien 29 May Fitting the luminosity data from type Ia supernovae by means of the.
The Meaning of Einstein’s Equation*
General Relativity and Cosmology The End of Absolute Space Cosmological Principle Black Holes CBMR and Big Bang.
New variables for brane-world gravity László Á. Gergely University of Szeged, Hungary Albert Einstein Century Internatonal Conference, Paris, 2005 Early.
Has elasticity anything to do with cosmology? Angelo Tartaglia RELGRAV.
The Expanding Universe
Announcements Final exam is Monday, May 9, at 7:30 am. –Students with last names A-K go to 225 CB. –Students with last names L-Z go to 300 CB. –All students.
Do consistent modified gravity models mimic General Relativity? S. Appleby, R. Battye. Talk based on arXiv:
The Fate of the Universe. The fate depends on the rate of expansion and the density Density greater than critical value – gravity will halt expansion.
ETSU Astrophysics 3415: “The Concordance Model in Cosmology: Should We Believe It?…” Martin Hendry Nov 2005 AIM:To review the current status of cosmological.
Special Relativity (Math)  Reference from Tipler chapter 39-1 to 39-3  Newtonian relativity  Einstein’s postulates  Lorentz transformation  Time dilation.
Introduction: Big-Bang Cosmology
Conclusion of Last Class: Hubble’s Law (that far away galaxies recede faster) implies that the universe is expanding uniformly in all directions, like.
Expansion of the Universe
Quantum Spacetime and Cosmic Inflation
Expressing n dimensions as n-1
Presentation transcript:

TeVPA08 Beijing -24 September Space-time defects and the accelerated expansion of the universe: an alternative to dark energy? Angelo Tartaglia DIFIS – Politecnico and INFN Torino, Italy

TeVPA08 Beijing -24 September Plan of the talk Starting point and motivation Starting point and motivation Outline of the Cosmic Defect theory Outline of the Cosmic Defect theory Fit of the observational data Fit of the observational data Open problems Open problems

TeVPA08 Beijing -24 September Inflation Gravity in clusters and galaxies Accelerated expansion There is something missing Modify GR Introduce new fields in standard GR Give up GR and look for another theory Puzzles of standard cosmology

TeVPA08 Beijing -24 September Accept a four- (N-) dimentional spacetime manifold Add “matter” components Isotropy and homogeneity Perfect fluid

TeVPA08 Beijing -24 September Λ Cold Dark Matter Simplest and most effective model for the universe; however: “matter” must be 7 times more than what we “see” (~30% of the cosmic source); Λ corresponds to 70% of the cosmic souce but … what is Λ?

TeVPA08 Beijing -24 September The Cosmic Defect theory: strain in a continuum N-dimensional “sheet” Strain induced by boundary conditions Elasticity

TeVPA08 Beijing -24 September A defect Internal “spontaneous” strain state

TeVPA08 Beijing -24 September Geometry, elasticity and defects Reference manifold Natural manifold

TeVPA08 Beijing -24 September In a strained medium each point is in one to one correspondence with points in the unstrained state In the purely elastic case the new situation is diffeomorphic to the old one  may be expressed as a function of x as well as of ξ Intrinsic coordinatesExtrinsic coord. Displacement

TeVPA08 Beijing -24 September Induced metric Strain tensor (represented in the reference manifold)

TeVPA08 Beijing -24 September “Radial” displacement field (space isotropy and homogeneity) Strained

TeVPA08 Beijing -24 September A Robertson-Walker universe

TeVPA08 Beijing -24 September How can we choose a Lagrangian expressing the presence of the defect? Start from the phase space of a Robertson-Walker universe and look around for similar phase spaces

TeVPA08 Beijing -24 September Phase space analogy FRW universe Inertial expansion Accelerated expansion Decelerated expansion Point particle Free motion Driving force Braking force

TeVPA08 Beijing -24 September A simple classical problem Motion of a point massive particle in a viscous medium

TeVPA08 Beijing -24 September Spacetime “Dissipative” action integral Same structure as in the classical simple case The “viscous” properties of space-time are contained in the vector field 

TeVPA08 Beijing -24 September Impose the 4-isotropy around the origin and use cosmic time as the “radial” coordinate

TeVPA08 Beijing -24 September Symmetry and application of the minimal action principle do not commute Defect means Symmetry first

TeVPA08 Beijing -24 September Divergence free vector

TeVPA08 Beijing -24 September Expansion rate Accelerated expansion Asymptotic stop

TeVPA08 Beijing -24 September Expansion versus cosmic time Inflation Acceleration

TeVPA08 Beijing -24 September Fitting the data from SnIa One has to account for the presence of matter

TeVPA08 Beijing -24 September Distance modulus vs z (192 SnIa)

TeVPA08 Beijing -24 September ΛCDM  2 = CD  2 = Reduced  2 of the fits

TeVPA08 Beijing -24 September The Hubble parameter H 0 = (62.8 ± 1.7) km/s  Mpc Most models ~64 km/s  Mpc Observation~75 km/s  Mpc

TeVPA08 Beijing -24 September Weaknesses and open problems Fitting the SnIa luminosity data with a logarithmic function and two parameters is “too easy” Fitting the SnIa luminosity data with a logarithmic function and two parameters is “too easy” The heuristic definition of the Lagrangian (though working) needs more stringent arguments: why is it working? The heuristic definition of the Lagrangian (though working) needs more stringent arguments: why is it working?

TeVPA08 Beijing -24 September The null divergence condition should be a consequence of the singularity in correspondence of the defect, rather than a formal constraint imposed on the vector. The null divergence condition should be a consequence of the singularity in correspondence of the defect, rather than a formal constraint imposed on the vector.

TeVPA08 Beijing -24 September Correspondences Defect theory in solids Defect theory in solids Bimetric theories: “pre-shaped container” Bimetric theories: “pre-shaped container” Vector-tensor theories Vector-tensor theories Curvature fluid Curvature fluid

TeVPA08 Beijing -24 September Final remarks The CD theory provides a consistent physical interpretation of space-time giving a heuristic tool to move across the Lagrangian “forest” set up by Lagrangian “engineering” mostly driven by the formal search for the desired result. This conceptual framework looks promising

TeVPA08 Beijing -24 September A. Tartaglia, M. Capone, Int. Jour. Mod. Phys. D, 17, (2008) A. Tartaglia, N. Radicella, Phys. Rev. D, 76, (2007) A. Tartaglia, M. Capone, V. Cardone, N. Radicella, arXiv: , to appear on Int. Jour. Mod. Phys. D arXiv:

TeVPA08 Beijing -24 September VII Friedmann Seminar João Pessoa 1 July

TeVPA08 Beijing -24 September …. according to the general theory of relativity space is endowed with physical qualities; in this sense, therefore, there exists an ether. ….. But this ether may not be thought of as endowed with the quality characteristic of ponderable media, as consisting of parts which may be tracked through time. The idea of motion may not be applied to it. Albert Einstein, Leiden, 1920 Ether again

TeVPA08 Beijing -24 September Some history “Ether is a very wonderful thing. It may exist only in the imagination of the wise, being invented and endowed with properties to suit their hypotheses; but we cannot do without it. How is energy to be transmitted through space without a medium?” Oliver Heaviside, Electrical Papers, 1892

TeVPA08 Beijing -24 September The introduction of a “luminiferous ether” will prove to be superfluous inasmuch as the view here to be developed will not require an “absolutely stationary space”….. Albert Einstein, 1905 Ether is superfluous

TeVPA08 Beijing -24 September The cosmological constant “Much later, when I was discussing cosmological problems with Einstein, he remarked that the introduction of the cosmological term was the biggest blunder of his life. ----” George Gamow, My World Line, 1970