far-from-equilibrium isotropisation , quasi-normal modes and radial flow
DESCRIPTION
Work with Michał Heller, David Mateos, Michał Spalinski, Diego Trancanelli and Miquel Triana References: 1202.0981 (PRL 108) and 1210.xxxx. Far-from-equilibrium isotropisation , quasi-normal modes and radial flow. Wilke van der Schee Supervisors: Gleb Arutyunov, Thomas Peitzmann, - PowerPoint PPT PresentationTRANSCRIPT
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FAR-FROM-EQUILIBRIUM ISOTROPISATION, QUASI-NORMAL
MODES AND RADIAL FLOWComparing numerical evolution with
linearisation
Wilke van der Schee
Supervisors: Gleb Arutyunov, Thomas Peitzmann, Koenraad Schalm and Raimond Snellings
Workshop Holographic Thermalization, LeidenOctober 11, 2012
Work with Michał Heller, David Mateos, Michał Spalinski, Diego Trancanelli and Miquel Triana
References: 1202.0981 (PRL 108) and 1210.xxxx
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Outline
Simple set-up for anisotropy
Quasi-normal modes and linearised evolution
Radial flow (new results, pictures only)
2/19
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Simplest set-up: Pure gravity in AdS5
Background field theory is flat Translational- and SO(2)-invariant field theory
We keep anisotropy: Caveat: energy density is constant so final state is
known
Holographic context3/19
P.M. Chesler and L.G. Yaffe, Horizon formation and far-from-equilibrium isotropization in supersymmetric Yang-Mills plasma (2008)
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The geometry4/19
Symmetry allows metric to be:
A, B, are functions of r and t B measures anisotropy
Einstein’s equations simplify Null coordinates Attractive nature of horizon
Key differences with Chesler, Yaffe (2008) are Flat boundary Initial non-vacuum state
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The close-limit approximation5/
19
Early work of BH mergers in flat space
Suggests perturbations of an horizon are always small
Linearise evolution around final state (planar-
AdS-Schw):
Evolution determined by single LDE:
R. H. Price and J. Pullin, Colliding black holes: The Close limit (1994)
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Quasi-normal mode expansion6/
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Expansion:
Solution possible for discrete Imaginary part always positive
G.T. Horowitz and V.E. Hubeny, Quasinormal Modes of AdS Black Holes and the Approach to Thermal Equilibrium(1999)J. Friess, S. Gubser, G. Michalogiorgakis, and S. Pufu, Expanding plasmas and quasinormal modes of anti-de Sitter black holes (2006)
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7
First results (Full/Linearized/QNM)
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Bouncing off the boundary8/19
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IR, normal, UV9/
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Statistics of 2000 profiles10/19
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Recent additions11/19
Same linearised calculations with a boost-invariant direction Subtlety: final state is not known initially Add-on: non-homogeneous and includes
hydrodynamics Works well
Second and third order corrections The expansion seems to converge Works quite well
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Radial flow12/19
Calculation incorporating longitudinal and radial expansion
Numerical scheme very similar to colliding shock-waves: Assume boost-invariance on collision axis Assume rotational symmetry (central collision) 2+1D nested Einstein equations in AdS
P.M. Chesler and L.G. Yaffe, Holography and colliding gravitational shock waves in asymptotically AdS5 spacetime (2010)
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Radial flow – initial conditions
13/19
Two scales: T and size nucleus Energy density is from Glauber model
(~Gaussian) No momentum flow (start at ~ 0.05fm/c) Scale solution such that Metric functions ~ vacuum AdS (not a solution
with energy!)
fm/catMeV 6.0506 T
H. Niemi, G.S. Denicol, P. Huovinen, E. Molnár and D.H. Rischke, Influence of the shear viscosity of the quark-gluon plasma on elliptic flow (2011)
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Radial flow – results14/19
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Radial flow - acceleration15/19
Velocity increases rapidly:
Acceleration is roughly with R size nucleus Small nucleus reaches maximum quickly
g3110
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Radial flow – energy profile16/19
Energy spreads out:
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Radial flow - hydrodynamics17/19
Thermalisation is quick, but viscosity contributes
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Radial flow - discussion18/19
Radial velocity at thermalisation was basically unknown
Initial condition is slightly ad-hoc, need more physics? We get reasonable pressures Velocity increases consistently in other runs Results are intuitive
Input welcome
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Conclusion19/19
Studied (fast!) isotropisation for over 2000 states UV anisotropy can be large, but thermalises fast
(though no bound)
Linearised approximation works unexpectedly well Works even better for realistic and UV profiles
Numerical scheme provides excellent basis Radial flow, fluctuations, elliptic flow What happens universally? What is the initial state?