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С MB anisotropy induced by a moving straight cosmic string. Sternberg State Astronomical Institute of Moscow State University. Sazhina O.S. Sazhin M.V. Sementsov V.N. Capaccioli M. Longo G. Riccio G. 15 th International Seminar on High Energy Physics QUARKS’2008 Sergiev Posad, Russia - PowerPoint PPT Presentation
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СMB anisotropy induced by a moving straight cosmic string
Sazhina O.S.Sazhin M.V.Sementsov V.N.Capaccioli M.Longo G.Riccio G.
Sternberg State Astronomical Institute of Moscow State University
15th International Seminar on High Energy Physics QUARKS’2008
Sergiev Posad, Russia May 23-29, 2008
The main results It was elaborated the method of searching
for cosmic strings based on analysis of the CMB anisotropy;
Moving straight cosmic string was shown to generate distinctive structures of enhanced and reduced temperature fluctuations on the surface of last scattering;
It was analized the conditions under which a cosmic string could be detected by both CMB anisotropy and gravitational lensing.
A
B A B
Euclidean Universe
Conical Universe
2
Rl2
Rl2
Cosmic string in the UniverseСosmic strings have been introduced in theoretical cosmology by Kibble, 1976; Zeldovich, 1980; Vilenkin, 1981
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0,1,1,0'ln8
1,1,1,1
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Cosmic string in the Universe
1,1,1,1ˆ diagg
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Cosmic string in the Universe
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1,1,1,1ˆ diagg
Deficit angle
Cosmic string in the UniverseThe conical Universe is equivalent to euclidean Universe with cut
The cosmic string status in modern theoretical cosmologyAmong all possible types of topological defects, cosmic strings are particulary interesting and their existence finds support in superstring theories, both in compactification models and in theories with extended additional dimensions;
From theoretical point of view for cosmic strings it is available the large mass range: from the GUT to electroweak energies.
fundamental strings of
superstring theory
cosmic strings
The energy scale for cosmic strings is the scale of GUT or less
The energy scale for fundamental strings is Planck scale
GeV15102GeV1910
cosmic strings
fundamental strings of
superstring theory
GeV1910Such heavy strings do not exist in our Universe today, and cannot have played any role in cosmological evolution except in the first few Planck times
cosmic strings
fundamental strings of
superstring theory
GeV1510
GeV1910Now we know models with large compact dimensions, in which the string scale may be much lower, down to the GUT scale or even less.
cosmic strings
fundamental strings of
superstring theory
Branes, which now play key role in superstring theory, can collide and generate cosmic strings.
cosmic strings branes
The cosmic string status in modern observational cosmologyThe current CMBR data exclude cosmic strings as source of primordial density perturbations. The data give the upper bound on the mass of cosmic strings but do not forbid their existence.
The methods were oriented to search string networks only, not individual strings as we now proposed.
The foreground-reduced internal linear combination map based on the 5 year WMAP data
The temperature power spectrum based on the 5 year WMAP data
Modern methods of cosmic string detection Optical surveys
Looking for gravitational lensing events
Radio surveys
The investigations of the structure of CMB anisotropy
Gravitational radiation from string loops
Interaction of string and black hole
Decay of heavy particles emitted by string
String + string interaction ...
The investigations of the structure of CMB anisotropy looking for cosmic string footprints
Looking for gravitational lensing events induced by cosmic string
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The cosmological model in use
The simplу simulation of a straight cosmic string moving with constant velocity
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CMB anisotropy induced by straight moving cosmic string
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CMB anisotropy induced by straight moving cosmic string. Results of preliminary simulations.
R – distance from observer to string (in units of SLS);
v – string velocity (in units of c); ψ – direction angle between line of sight
and velocity of string.
(R,v,ψ)
(R,v,ψ)=(0.9,0.9,90°)
v
(R,v,ψ)=(0.5,0.9,90°)
(R,v,ψ)=(0.1,0.9,90°)
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Time retardation over the string extension (A.Vilenkin, 1986)
If an infinite straight string moves past the observer, he sees its distant parts with a retardation, so that the string appears to him to be curved
OSzOOR
A '
R=0.15 v=0.1 ψ=90°with retardation
R=0.15 v=0.4 ψ=90°with retardation
R=0.15 v=0.7 ψ=90°with retardation
(R,v,ψ)=(0.9,0.9,90°)
(R,v,ψ)=(0.9,0.5,90°)
(R,v,ψ)=(0.9,0.1,90°)
(R,v,ψ)=(0.9,0.9,45°)
(R,v,ψ)=(0.9,0.9,90°)
(R,v,ψ)=(0.9,0.9,120°)
KTT
KTT
5.11.0
1006
The low observational limit due the available resolution (Hubble Space Telescope) in optical searching of gravitational lensing events of galaxies by cosmic strings. “Superlight” strings could exist but can not be detected.
The upper bound on string deficit angle. The induced anisotropy (amplitude of spot) is compared with anisotropy due adiabatic fluctuations and could be detected.
Why strings with deficit angle more than 10” does not exist? Because we do not observe such structures.
50°
100°
150°
200°
0°z=0 z=2 z=4 z=6 z=8
spoth
7z
1000z
spoth
%20
Minimal string number N ~ 10Maximal string number N ~ 1000
Main conclusions We found the structure of the CMB anisotropy generated on a
cosmic string for simple model of straight string moving with constant velocity;
The number of strings that could be detected by optical method is only 20%, therefore the gravitational lensing method has to be “completed” by CMB one;
For strings with deficit angle 1-2 arcsec the amplitude of generated anisotropy has to be 15-30 microK (the corresponding string linear density is and energy is GUT one, );
To use both radio and optical methods the deficit angle has to be from 0.1 arcsec to 5-6 arcsec.
If cosmic string could be detected by optical method, the hight of corresponding brightness spot of anisotropy has to be no less than 100°.
710~ G GeV1510
Thank you for attention