Joan Solà (UB) (TeVPA 08 ).

Slides:



Advertisements
Similar presentations
Modeling nonlinear dark energy fluctuations Ronaldo Carlotto Batista IF-USP Raul Abramo, Rogério Rosenfeld, Lamartine Liberato I Workshop: Challanges of.
Advertisements

Benasque 2012 Luca Amendola University of Heidelberg in collaboration with Martin Kunz, Mariele Motta, Ippocratis Saltas, Ignacy Sawicki Horndeski Lagrangian:
1/03/09 De 89 à 98. 1/03/09 De 89 à 98 1/03/09 De 89 à 98.
Dark Energy. Conclusions from Hubble’s Law The universe is expanding Space itself is expanding Galaxies are held together by gravity on “small” distance.
Testing CPT with CMB 李明哲 University of Bielefeld 2008 年 4 月 28 日.
José Beltrán and A. L. Maroto Dpto. Física teórica I, Universidad Complutense de Madrid XXXI Reunión Bienal de Física Granada, 11 de Septiembre de 2007.
Quintessence from time evolution of fundamental mass scale.
The Consequences of a Dynamical Dark Energy Density on the Evolution of the Universe By Christopher Limbach, Alexander Luce, and Amanda Stiteler Background.
Dark Energy Perturbations 李明哲 南京大学物理学院 中国科技大学交叉学科理论研究中心 合肥.
18 The Big Bang Where do we come from, where are we going?
The Opposite of Dark Energy: Limits on Ultralight Energy in the Early Universe Robert J. Nemiroff Michigan Technological University.
Quintessence – Phenomenology. How can quintessence be distinguished from a cosmological constant ?
Concepts from Modern Physics. Relativity We experience space in 4 dimensions (but we’re now pretty sure there’s more of them). We can’t go faster than.
Dark Energy: “The Anti-Gravity” Joseph C. Brossett.
Cosmology, Inflation & Compact Extra Dimensions Chad A. Middleton Mesa State College March 1, 2007 Keith Andrew and Brett Bolen, Western Kentucky University.
Inflation and the Early Universe 早期宇宙之加速膨脹 Lam Hui 許林 Columbia University.
Modern Physics Modern Physics Global Mechanics Global Mechanics Astrophysics Astrophysics Cosmology and The Little Bang Cosmology and The Little Bang.
The physics of inflation and dark energy 1.3 Dark energy: some evidence (short list) Ages of glob. clusters/galaxies at z~2-3:  m 0.6 SN Ia:   -
Dark Energy. Expanding Universe Galaxies in the universe are spreading out over time. –Hubble’s law From Einstein’s general relativity this happens as.
DARK MATTER AND DARK ENERGY This powerpoint will show you the basics of dark matter and dark energy Their place in the universe By Jordan Ilori.
Holographic and agegraphic dark energy models Yun Soo Myung Inje University, Gimhae, Korea.
Credit: O. Krause (Steward Obs.) et al., SSC, JPL, Caltech, NASA South Africa and the SDSS-II Supernova Survey Ed Elson (SAAO/NASSP) Bruce Bassett (SAAO/ICG)
General Relativity Physics Honours 2008 A/Prof. Geraint F. Lewis Rm 560, A29 Lecture Notes 10.
Neutrino Models of Dark Energy LEOFEST Ringberg Castle April 25, 2005 R. D. Peccei UCLA.
Marco Bruni, ICG, University of Portsmouth & Dipartimento di Fisica, Roma ``Tor Vergata” Paris 8/12/05 Dark energy from a quadratic equation of state Marco.
ERE 2008September 15-19, Spanish Relativity Meeting 2008, Salamanca, September (2008) Avoiding the DARK ENERGY coincidence problem with a COSMIC.
Interacting Dark Energy Xinmin Zhang Institute of High Energy Physics Beijing Outline of the talk I. Current constraints on Dark Energy a. Constraints.
Effects of Dynamical Compactification on d-Dimensional Gauss-Bonnet FRW Cosmology Brett Bolen Western Kentucky University Keith Andrew, Chad A. Middleton.
Degenerate neutrino as a Dark Energy 12 th Marcel Grossmann Meeting, July 2009, Paris Hyung Won Lee, Inje University July 15, 2009 Collaboration.
Neutrino Model of Dark Energy Yong-Yeon Keum Academia Sinica/Taiwan Mujuresort, Feb./16-19/2005.
Cosmology (Chapter 14) NASA. Student Learning Objectives Describe the Big Bang theory Analyze possible fates of our universe.
Dark Energy in the Early Universe Joel Weller arXiv:gr-qc/
Salient Features of the Universe Homogeneity and isotropy for 6000 Mpc > x > 100 Mpc Universe expanding uniformly ordinary matter is more abundant than.
Quintessence Dark Energy & Acceleration of the Universe B URIN G UMJUDPAI The Tah Poe Academia Institute for Theoretical Physics & Cosmology Department.
DARK ENERGY. EXPANSION OF THE UNIVERSE Early 1990’s – Universal expansion expected to slow - Universe is full of matter, and gravity pulls matter together.
L. Perivolaropoulos Department of Physics University of Ioannina Open page.
HEPont.rdf Kirsten Sachs AAHEP7 April 3, 2014 HEP astro nucl ins-det acc-ph cs math cond-mat data-an general
Dark Energy vs. Dark Matter Towards a unification… Centre de Recherche Astronomique de Lyon Alexandre ARBEY March 5, 2006.
Where is the Universe?. Cosmological Questions Temporal Temporal Spatial Spatial Compositional Compositional Teleological Teleological Behind physics.
Determination of cosmological parameters Gong-Bo Zhao, Jun-Qing Xia, Bo Feng, Hong Li Xinmin Zhang IHEP, Beijing
Cosmology Lecture 10 The early universe. Our benchmark universe (  CDM) H 0 = 72 km s -1 Mpc -1  0 = 1 - spatially flat   = 0.73  m = 0.27  m,baryon.
Cosmology of Non-Hermitian (C)PT-invariant scalar matter A.A. Andrianov Universitat de Barcelona( ECM & ICC) & St.Petersburg State University Discrete2008,
The Big Bang.  Cosmology – The study of the structure and evolution of the universe.  Big Bang Theory – The universe was very hot and small. Billions.
。 33 投资环境 3 开阔视野 提升竞争力 。 3 嘉峪关市概况 。 3 。 3 嘉峪关是一座新兴的工业旅游城市,因关得名,因企设市,是长城文化与丝路文化交 汇点,是全国唯一一座以长城关隘命名的城市。嘉峪关关城位于祁连山、黑山之间。 1965 年建市,下辖雄关区、镜铁区、长城区, 全市总面积 2935.
Modern Theories of the Universe The final work EVA OPATŘILOVÁ 2015.
Phantom Dark Energy Zong-Kuan Guo (advisor: Yuan-Zhong Zhang)
FAILURES OF HOMOGENEOUS & ISOTROPIC COSMOLOGIES IN EXTENDED QUASI-DILATON MASSIVE GRAVITY (arXiv: ) Saurabh Kumar, Department of Physics, Case.
Work, Energy, Kinetic Energy and the Conservation of Energy
January 29, 2003 Science Center 308 3:00 p.m.
Quiz Review Describe energy Describe work
Observational Constraints on the Running Vacuum Model
Interacting Dark Energy
``Welcome to the dark side of the world.”
The role of potential in the ghost-condensate dark energy model
Probing the Coupling between Dark Components of the Universe
Astronomy Picture of the Day (2007 Oct. 21)
The Law of Conservation of Matter/Mass
Pop-quiz #9 Which of the following statements is TRUE?
أنماط الإدارة المدرسية وتفويض السلطة الدكتور أشرف الصايغ
The Stability Issue In Models Of Neutrino Dark Energy
Coincidence Problem in Interacting Dark energy model
مديريت موثر جلسات Running a Meeting that Works
The Big 6 Research Model Step 3: Location and Access
Non Singular Origin of the Universe and its Present Va-cuum Energy Density, IJMPA & Honorable Mention in Gravity Research Foundation Competition for 2011,
Outstanding Problems in Cosmology
Void alignment and density profile applied to measuring cosmological parameters Speaker: De-Chang Dai MNRAS (4): (arXiv: )
Tev particle astrophysics at IHEP
Graduate Course: Cosmology
Local Conservation Law and Dark Radiation in Brane Models
Energy Transformations and Conservation
Presentation transcript:

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Some recent works on ``Running Cosmology’’ Joan Solà (UB) (TeVPA 08 )

First works Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

91-years-old Cosmological Constant Problem !! Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

(unmixed conservation laws) Dynamical Dark Energy (unmixed conservation laws) Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

! Nice feature of quintessence field: Problems with quintessence field: ! Joan Solà (UB) (TeVPA 08 )

With phantoms the situation is worst: ``Big Rip’’ Joan Solà (UB) (TeVPA 08 )

Mixed possibilities: Joan Solà (UB) (TeVPA 08 )

! Various Forms of DE versus matter radiation matter quintessence ``Big Rip’’ phantom matter phantom DE ! Joan Solà (UB) (TeVPA 08 )

!! Joan Solà (UB) (TeVPA 08 )

Running cosmological ``constant’’ Joan Solà (UB) (TeVPA 08 )

!! Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

``Running’’ cosmology (mixed conservation law!) Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Joan Solà (UB) (TeVPA 08 )

Conclusions Joan Solà (UB) (TeVPA 08 )