Dark Energy: Hopes and Expectations Mario Livio Space Telescope Science Institute Mario Livio Space Telescope Science Institute.

Slides:



Advertisements
Similar presentations
The Nuts and Bolts of Inflation Richard Barrett. Dark Energy SeminarGlasgow 29/11/2003 Inflation What is inflation? What is dark energy? Why was inflation.
Advertisements

Quantum One: Lecture 1a Entitled So what is quantum mechanics, anyway?
Theories of gravity in 5D brane-world scenarios
Richard Kenway Everything is a computer Richard Kenway.
P ROBING SIGNATURES OF MODIFIED GRAVITY MODELS OF DARK ENERGY Shinji Tsujikawa (Tokyo University of Science)
Cosmodynamics. Quintessence and solution of cosmological constant problem should be related !
Tony Liss Saturday Physics for Everyone November 9, 2013 (With debts to Chris Quigg, Leonard Susskind, Hitoshi Murayama)
String/Brane Cosmology …for those who have not yet drunk the Kool-Aid C.P. Burgess with J.Blanco-Pillado, J.Cline, C. de Rham, C.Escoda, M.Gomez-Reino,
Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab, UCL 10. Inflation.
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.
Quintessence from time evolution of fundamental mass scale.
Probing the Structure of Stringy Landscape by Large Scale CMB Experiments Amjad Ashoorioon in collaboration with Ulf H. Danielsson 24 th Nordic Conference.
Physical Constraints on Gauss-Bonnet Dark Energy Cosmologies Ishwaree Neupane University of Canterbury, NZ University of Canterbury, NZ DARK 2007, Sydney.
Astronomy and Cosmologies Wed.18.May 2005, last lecture, Spring 2005, Zita Age of the universe – finish H workshop Your questions on Cosmology and the.
Coupled Dark Energy and Dark Matter from dilatation symmetry.
Adventures in String Theory Science One, April 7 th, 2011.
Macroscopic Behaviours of Palatini Modified Gravity Theories [gr-qc] and [gr-qc] Baojiu Li, David F. Mota & Douglas J. Shaw Portsmouth,
Voids of dark energy Irit Maor Case Western Reserve University With Sourish Dutta PRD 75, gr-qc/ Irit Maor Case Western Reserve University With.
Chiral freedom and the scale of weak interactions.
Program 1.The standard cosmological model 2.The observed universe 3.Inflation. Neutrinos in cosmology.
Quintessence from time evolution of fundamental mass scale.
Astro-2: History of the Universe Lecture 11; May
Phenomenology of bulk scalar production at the LHC A PhD oral examination A PhD oral examination By Pierre-Hugues Beauchemin.
Astro-2: History of the Universe Lecture 9; May
Large distance modification of gravity and dark energy
Dark Energy and Modified Gravity IGC Penn State May 2008 Roy Maartens ICG Portsmouth R Caldwell.
Modified (dark) gravity Roy Maartens, Portsmouth or Dark Gravity?
Relic Neutrinos as a Source of Dark Energy Neal Weiner New York University IDM04 R.Fardon, D.B.Kaplan, A.E.Nelson, NW What does dark energy have to do.
 It would appear that there is more matter in the universe, called dark matter, than we see. We believe this because  The edges of galaxies are rotating.
Lecture 3: Modified matter models of dark energy Shinji Tsujikawa (Tokyo University of Science)
Dilaton quantum gravity and cosmology. Dilaton quantum gravity Functional renormalization flow, with truncation :
STANDARD COSMOLOGY; PROBLEMS AND THEIR SOLUTIONS KUMAR ATMJEET (UNIV. OF DELHI) SUPERVISOR: T. SOURADEEP IUCAA, PUNE (May-July, 2006)
Dilaton quantum gravity and cosmology. Dilaton quantum gravity Functional renormalization flow, with truncation :
Intro to Cosmology! OR What is our Universe?. The Latest High Resolution Image of the Cosmic Microwave Background Radiation Low Energy RegionHigh Energy.
Seesaw for the Higgs boson Xavier Calmet Université Libre de Bruxelles.
1 Dark Energy & MSSM Jérôme Martin Institut d’Astrophysique de Paris (IAP)
The false vacuum bubble : - formation and evolution - in collaboration with Chul H. Lee(Hanyang), Wonwoo Lee, Siyong Nam, and Chanyong Park (CQUeST) Based.
Physical Foundations of Natural Science Vasily Beskin # 2-4.
Dark Energy In Hybrid Inflation Seongcheol Kim (KAIST) Based on Phys. Rev. D75: (2007)
PHY th century cosmology 1920s – 1990s (from Friedmann to Freedman)  theoretical technology available, but no data  20 th century: birth of observational.
Neutrino Models of Dark Energy LEOFEST Ringberg Castle April 25, 2005 R. D. Peccei UCLA.
1 Wavefunction of the Universe on the Landscape of String Theory Laura Mersini-Houghton UNC Chapel Hill, USA.
A MANIFESTLY LOCAL T HEORY OF V ACUUM E NERGY S EQUESTERING George Zahariade UC Davis.
The Higgs Boson Observation (probably) Not just another fundamental particle… July 27, 2012Purdue QuarkNet Summer Workshop1 Matthew Jones Purdue University.
Cosmology and Dark Matter IV: Problems with our current picture Jerry Sellwood.
Holographic Dark Energy and Anthropic Principle Qing-Guo Huang Interdisciplinary Center of Theoretical Studies CAS
Cosmological Constant in the Multiverse Vladimir Burdyuzha Astro-Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Moscow Miami-2008,
Can observations look back to the beginning of inflation ?
Neutrino Model of Dark Energy Yong-Yeon Keum Academia Sinica/Taiwan Mujuresort, Feb./16-19/2005.
“Planck 2009” conference Padova May 2009 Facing Dark Energy in SUGRA Collaboration with C. van de Bruck, A. Davis and J. Martin.
Lecture 27: The Shape of Space Astronomy Spring 2014.
Dark Energy at Future Colliders: Testing the True Nature of Dark Energy in Black Hole Evaporations Jörg Jäckel Rencontres des Moriond March 2005 Michael.
Gravity effects to the Vacuum Bubbles Based on PRD74, (2006), PRD75, (2007), PRD77, (2008), arXiv: [hep-th] & works in preparation.
Cosmology in Eddington- inspired Born-Infeld gravity Hyeong-Chan Kim Korea National University of Transportation 19 Feb 2013 The Ocean Suites Jeju, Asia.
ETSU Astrophysics 3415: “The Concordance Model in Cosmology: Should We Believe It?…” Martin Hendry Nov 2005 AIM:To review the current status of cosmological.
The Nature of Dark Energy David Weinberg Ohio State University Based in part on Kujat, Linn, Scherrer, & Weinberg 2002, ApJ, 572, 1.
In Dynamic Dark Energy Models. 1. Accelerating expansion & interpretation 2. What is Dynamic dark energy model 3. recent observational results.
The HORIZON Quintessential Simulations A.Füzfa 1,2, J.-M. Alimi 2, V. Boucher 3, F. Roy 2 1 Chargé de recherches F.N.R.S., University of Namur, Belgium.
Spherical Collapse and the Mass Function – Chameleon Dark Energy Stephen Appleby, APCTP-TUS dark energy workshop 5 th June, 2014 M. Kopp, S.A.A, I. Achitouv,
Theoretical Particle Physics Group (TPP)
Dark Energy: Hopes and Expectations
Long distance modifications of gravity in four dimensions.
Recent status of dark energy and beyond
dark matter Properties stable non-relativistic non-baryonic
Supersymmetry, naturalness and environmental selection
Stealth Acceleration and Modified Gravity
Shintaro Nakamura (Tokyo University of Science)
cosmodynamics quintessence fifth force
Presentation transcript:

Dark Energy: Hopes and Expectations Mario Livio Space Telescope Science Institute Mario Livio Space Telescope Science Institute

What Causes Cosmic Acceleration? 1.Dark Energy? 2.Standard General Relativity? 3.Alternative Theories of Gravity?

Standard GR? Premise:Universe not homogeneous today (fractal bubble model). Result:Non-linear gravitational effects, averages, local time => distance-redshift relation as observed. Strengths:1. No need for unseen stuff. 2. No need to change GR. 3. Could perhaps be resolved soon. Problems: 1. Anti-Copernican (Milky Way in special place)? (Not necessarily, but different angular scales in CMB.) 2. Not clear if solution can match all observations (e.g. H 0, peaks in CMB).

Dark Energy vs. Alternative Gravity Theory Dark Energy 1.Vacuum energy (cosmological constant), w = const. = -1 2.Scalar field, w can vary from w < -1 to w = 1 Alternative Gravity 1.Modification of Friedmann equation (5D gravity). Analogous to: w = -½ in distant past, evolving to w = -1 in distant future. 2.Purely phenomenological modifications to the GR Lagrangian.

Alternative Gravity Strengths: 1. Motivated by ideas from string theory. 2. Testable in principle. Weaknesses: 1. All but ruled out by lab and lunar ranging experiments Inverse square law holds down to d = 56  m! Measurements of lunar perihelion precession with an accuracy of δΦ = 1.4x10 -12

Alternative Gravity cont’d Yellow region excluded at 95% confidence level. 2. Not clear if self- consistent model exists.

Vacuum Energy Strengths: 1. Clearly exists! 2. If dark energy behaves like an ideal fluid: This is unstable for any negative value of w, except w = -1, vacuum energy! Casimir Effect

Vacuum Energy (cont’d) Problems: 1. Why so small and positive? (But SUSY testable by LHC) 2. Why now?

Scalar Field Strengths: 1.Motivated by inflation. 3.The evolution of the field produces different w(z) behavior for “freezing” or “thawing” Observations can distinguish.

Scalar Field cont’d Weaknesses: 1.No convincing connections to inflation. 2.Does not really explain why small and why now. 3.Choice of potential, modifications to kinetic term, rather arbitrary. In thawing models  M ~  V just reflects mass of scalar field. 4.To produce acceleration, interaction of field with matter and with itself has to be extremely weak.

Cyclic Model with Dynamical Relaxation Cosmological constant  (t) very slowly varying function, most time spent at small and positive value.

Possibility of Multiverse? Inflation may produce an ensemble of pocket universes. Landscape scenario String theory suggests that ~ vacua may exist.

Possibility of Multiverse? Fundamental Theory All constants determined uniquely. Examples of past successes: 1.Particle masses in QCD 2.Electroweak theory Allows universes with an ensemble of values of at least some non-fundamental parameters. Examples of past non-fundamental quantities: 1.Number of planets in the Solar System 2.Shapes of snowflakes

Can A Multiverse Explain the Value of  V ? If  V can take a broad range of values in the multiverse, then complexity can arise only in some subuniverse. In general  V /  3 is constrained. For a flat probability distribution: Principle of mediocrity: Is our universe typical? By contrast, in cyclic model complexity can arise in almost every patch of space.

Typical Objections 1.Against the scientific method? Not everything should be observable or falsifiable. Rather, if the theory is testable in the observable universe, we should be prepared to accept its predictions in the unobservable parts. 2.No predictions? Not exactly true, statistical predictions. 3.End of physics? No. Rather, modification of expectations. E.g. in mathematics: Gödel’s theorem, computational complexity. 4.Supports religion-like arguments? Absolutely not!

Hopes and Expectations Scans? YesNo Symmetry and Dynamics Yes  QCD <<1 P, T violation, supersymmetric particles No , Q Masses of heavier quarks and leptons, weak mixing angles Dynamical and anthropic reasoning are not mutually exclusive! What should we do if multiverse is predicted?