Vortons: Dark Matter From Cosmic Strings

1999 ◽  
pp. 325-326
Author(s):  
C. J. A. P. Martins ◽  
E. P. S. Shellard
Keyword(s):  
Dark Matter ◽  
Cosmic Strings

scholarly journals Galaxy Formation with Hot Dark Matter and Cosmic Strings

1988 ◽  
Vol 130 ◽  
pp. 560-561
Author(s):  
Robert H. Brandenberger
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Cosmic Strings ◽  
Severe Problem ◽  
Small Scales ◽  
The Galaxy

Hot dark matter particles have large thermal velocities at teg and hence cannot be gravitationally bound on small scales (free streaming). In models of formation of structure based on linear adiabatic perturbations all inhomogeneities on scales smaller than the maximal free streaming length λj are washed out. The mass λj inside a bail of radius exceeds the galaxy mass. Hence in the above models galaxies can only lorm by fragmentation of larger-scale objects. This is a severe problem.

scholarly journals COSMIC STRINGS, LOOPS, AND LINEAR GROWTH OF MATTER PERTURBATIONS

2002 ◽  
Vol 11 (01) ◽  
pp. 61-102 ◽  
Author(s):  
JIUN-HUEI PROTY WU ◽  
PEDRO P. AVELINO ◽  
E. P. S. SHELLARD ◽  
BRUCE ALLEN
Keyword(s):  
Dark Matter ◽  
Structure Formation ◽  
Cosmic String ◽  
Cold Dark Matter ◽  
Cosmic Strings ◽  
Topological Analysis ◽  
Long Strings ◽  
Source Spectrum ◽  
Galaxy Surveys ◽  
Network Properties

We describe a detailed study of string-seeded structure formation using high resolution numerical simulations in open universes and those with a non-zero cosmological constant. We provide a semi-analytical model which can reproduce these simulation results including the effect from small loops chopped of by the string network. A detailed study of cosmic string network properties regarding structure formation is also given, including the correlation time, the topological analysis of the source spectrum, the correlation between long strings and loops, and the evolution of long-string and loop energy densities. For models with Γ=Ω h=0.1 -0.2 and a cold dark matter background, we show that the linear density fluctuation power spectrum induced by cosmic strings has both an amplitude at 8 h-1 Mpc, σ8, and an overall shape which are consistent within uncertainties with those currently inferred from galaxy surveys. The cosmic string scenario with hot dark matter requires a strongly scale-dependent bias in order to agree with observations.

scholarly journals FORMATION OF WAKES BY CHIRAL CONDUCTING COSMIC STRINGS

2004 ◽  
Vol 19 (32) ◽  
pp. 2445-2450 ◽  
Author(s):  
M. C. B. ABDALLA ◽  
A. A. BYTSENKO ◽  
M. E. X. GUIMARÃES
Keyword(s):  
Dark Matter ◽  
Cold Dark Matter ◽  
Cosmic Strings ◽  
Formation And Evolution

Chiral cosmic strings are naturally produced at the end of D-term inflation and they present very interesting cosmological consequences. In this work, we investigate the formation and evolution of wakes by a chiral string. We show that, for cold dark matter, the mechanism of forming wakes by a chiral string is similar to the mechanism by an ordinary string.

Cosmic strings with self-interacting hot dark matter

1998 ◽  
Vol 298 (1) ◽  
pp. 139-142 ◽  
Author(s):  
P. P. Avelino ◽  
J. P. M. de Carvalho
Keyword(s):  
Dark Matter ◽  
Cosmic Strings

scholarly journals Dark photon dark matter from a network of cosmic strings

2019 ◽  
Vol 99 (6) ◽  
Author(s):  
Andrew J. Long ◽  
Lian-Tao Wang
Keyword(s):  
Dark Matter ◽  
Cosmic Strings ◽  
Dark Photon

COSMIC STRINGS, HOT DARK MATTER AND THE LARGE-SCALE STRUCTURE OF THE UNIVERSE

1990 ◽  
Vol 05 (09) ◽  
pp. 1633-1651 ◽  
Author(s):  
ROBERT H. BRANDENBERGER ◽  
LEANDROS PERIVOLAROPOULOS ◽  
ALBERT STEBBINS
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Large Scale ◽  
Cosmic Strings ◽  
Unit Length ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Rotation Curves ◽  
The Universe

A review of recent results on large-scale structure and galaxy formation in a model with hot dark matter and cosmic strings is given. With cosmic strings seeding perturbations, many of the arguments against hot dark matter disappear. It is shown that spherical accretion about loops leads to dark matter haloes with flat velocity rotation curves. Velocity perturbations due to wakes behind long, moving strings lead to a network of planar overdensities with a distinguished scale of slightly less than 40×40 Mpc2. If the mass per unit length μ exceeds a certain bound, then the wakes become nonlinear by the present time. In this case, their thickness can be calculated.

scholarly journals Summary

1988 ◽  
Vol 130 ◽  
pp. 495-505
Author(s):  
P. J. E. Peebles
Keyword(s):  
Dark Matter ◽  
Large Scale ◽  
Cold Dark Matter ◽  
Cosmic Strings ◽  
Large Scale Structure ◽  
Observational Evidence ◽  
Scale Structure ◽  
Scale Invariant ◽  
The Real ◽  
Weak Points

This conference has been marked by our willingness to entertain grand schemes of synthesis of theoretical ideas and the observational evidence on how galaxies and large-scale structure might have formed. At IAU Symposium 104 on this subject held in Crete just 5 years ago there was little discussion of how all the pieces of the puzzle might fit together. Now we have at least three candidate grand syntheses that have been worked out in some detail and have been discussed here: scale-invariant cold dark matter, by Frenk; massive cosmic strings, by Turok; and exploding magnetized superconducting cosmic strings, by Ostriker. I have accordingly placed each of the topics I want to review under the heading of the grand scheme for which it seems most embarrassing. This negative approach is a little unfair, but I think we can take it as given that we would not be considering a scheme that did not have many good points, and that the real interest is the probing of weak points by which we hope to learn which schemes might be strengthened, which might safely be abandoned.

Sign in / Sign up

Export Citation Format

Share Document