scholarly journals On the Spherically Symmetric Solution of the Classical SU(2) Yang-Mills Field

1982 ◽  
Vol 68 (1) ◽  
pp. 261-276 ◽  
Author(s):  
Y. Miyachi ◽  
M. Ikeda ◽  
T. Maekawa
2009 ◽  
Vol 18 (04) ◽  
pp. 613-619 ◽  
Author(s):  
R. J. SLAGTER

We present a numerical solution on a five-dimensional spherically symmetric space–time, in Einstein–Yang–Mills — Gauss–Bonnet theory, using a two-point boundary value routine. It turns out that the Gauss–Bonnet contribution has a profound influence on the behavior of the particle-like solution: it increases the number of nodes of the YM field. When a negative cosmological constant is incorporated in the model, it turns out that there is no horizon and no singular behavior of the model. For a positive cosmological constant the model has singular behavior.


1970 ◽  
Vol 48 (2) ◽  
pp. 225-228 ◽  
Author(s):  
Leopold Halpern ◽  
Milivoj J. Miketinac

Møller's tetrad energy–momentum complex is made unique by introducing a suitable Yang–Mills field. The field equations are given and solved approximately for the spherically symmetric case. The simplest couplings to the K0 meson field are analyzed and it is shown that they cannot be used to resolve the CP violation.


1981 ◽  
Vol 59 (2) ◽  
pp. 283-288 ◽  
Author(s):  
J. W. Moffat

The predictions for the perihelion shift, the deflection of light, and the delay time of a light ray are calculated in the nonsymmetric theory of gravitation. An upper bound for the parameter l (that occurs as a constant of integration in the static, spherically symmetric solution of the field equations) is obtained for the sun for the experimental value of the perihelion shift of Mercury, yielding [Formula: see text]. The upper bound on [Formula: see text] obtained from the Viking spacecraft time-delay experiment is [Formula: see text]. For [Formula: see text], we find that the theory is consistent with the standard relativistic experiments for the solar system. The theory predicts that the perihelion of a satellite could reverse its direction of precession if it orbits close enough to the sun. The results for a highly eccentric satellite orbit are calculated in terms of the value [Formula: see text].


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