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VERSION:2.0
PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN
BEGIN:VEVENT
SUMMARY:Robinson–Trautman solutions in (2+1) dimensions
DTSTART:20220929T143000Z
DTEND:20220929T163000Z
DTSTAMP:20260722T172101Z
UID:d8228b16-1e59-40a0-8aef-044803d4e836
SEQUENCE:3
CREATED:20220923T215941Z
DESCRIPTION:Abstract:The Robinson-Trautman (RT) spacetime is the simplest 
 solution of General Relativity (GR) describing a compact source surrounded
  by gravitational waves. As an initial value problem\, the RT spacetime ev
 olution is a well-posed mathematical problem. The pertinent dynamical equa
 tions are equivalent to the so-called Calabi flow\, and regular initial da
 ta evolve smoothly towards a final state corresponding to a remnant Schwar
 zschild black hole. Extensions of RT spacetimes for higher dimensions (D &
 gt\; 4) were recently proposed\, and the essence of the RT evolution is un
 changed: regular initial data evolve towards a final higher-dimensional Sc
 hwarzschild black hole. The situation for D=3 is quite different due to so
 me peculiarities of low-dimensional GR. We will present a D=3 RT flow mimi
 cking the essential properties of the Calabi flow. In particular\, regular
  initial data evolve towards a final remnant BTZ black hole\, and any poss
 ible asymmetry in the initial data is expelled as a radiation fluid. 
LAST-MODIFIED:20220928T084240Z
LOCATION:Sala de Reuniões e Seminários do DF (2-8.3) (2nd Floor of Physi
 cs Building)
URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/robinsontrautman-solutions
 -in-21-dimensions/
X-ALT-DESC;FMTTYPE=text/html:<p data-block-key="jdpgh"><b>Abstract:</b><br
 />The Robinson-Trautman (RT) spacetime is the simplest solution of General
  Relativity (GR) describing a compact source surrounded by gravitational w
 aves. As an initial value problem\, the RT spacetime evolution is a well-p
 osed mathematical problem. The pertinent dynamical equations are equivalen
 t to the so-called Calabi flow\, and regular initial data evolve smoothly 
 towards a final state corresponding to a remnant Schwarzschild black hole.
  <br/><br/>Extensions of RT spacetimes for higher dimensions (D &gt\; 4) w
 ere recently proposed\, and the essence of the RT evolution is unchanged: 
 regular initial data evolve towards a final higher-dimensional Schwarzschi
 ld black hole. The situation for D=3 is quite different due to some peculi
 arities of low-dimensional GR. We will present a D=3 RT flow mimicking the
  essential properties of the Calabi flow. In particular\, regular initial 
 data evolve towards a final remnant BTZ black hole\, and any possible asym
 metry in the initial data is expelled as a radiation fluid. </p>
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