scholarly journals Galaxy Formation by Cosmic Strings and Cooling of Baryonic Matter

1987 ◽  
Vol 78 (6) ◽  
pp. 1219-1224 ◽  
Author(s):  
Mizuo Izawa ◽  
Humitaka Sato
1988 ◽  
Vol 130 ◽  
pp. 560-561
Author(s):  
Robert H. Brandenberger

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.


1986 ◽  
Vol 75 (6) ◽  
pp. 1342-1350 ◽  
Author(s):  
H. Sato

Author(s):  
H. A. Harutyunian

The physical mechanism of interaction between dark energy and ordinary baryonic matter is used to show that Ambartsumian's cosmogonic paradigm on the galaxy formation gets new support. This mechanism is considered to compare the cD galaxies observational properties with the model predictions in the framework of the suggested paradigm.


1988 ◽  
Vol 328 ◽  
pp. 23 ◽  
Author(s):  
Edmund Bertschinger ◽  
Paul N. Watts

1989 ◽  
Vol 571 (1 Texas Symposi) ◽  
pp. 151-169 ◽  
Author(s):  
EDMUND BERTSCHINGER

The role of strings in the early Universe is reviewed, with particular emphasis on the possibility that they may provide the fluctuations that lead to galaxy formation. Evidence from the correlation of clusters is presented. An alternative scenario, in which much lighter strings might come to dominate the recent Universe is also discussed briefly.


1990 ◽  
Vol 05 (09) ◽  
pp. 1633-1651 ◽  
Author(s):  
ROBERT H. BRANDENBERGER ◽  
LEANDROS PERIVOLAROPOULOS ◽  
ALBERT STEBBINS

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.


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