nonlinear field equations
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Optik ◽  
2018 ◽  
Vol 164 ◽  
pp. 460-464 ◽  
Author(s):  
Ruan-Jie Zhong ◽  
Xue-Long Zhang ◽  
Cheng-Lai Hu ◽  
Yue-Yue Wang ◽  
Chao-Qing Dai

2017 ◽  
Vol 32 (05) ◽  
pp. 1750039 ◽  
Author(s):  
Neven Bilić ◽  
Dragoljub D. Dimitrijevic ◽  
Goran S. Djordjevic ◽  
Milan Milosevic

We analyze the inflationary scenario based on the tachyon field coupled with the radion of the second Randall–Sundrum model (RSII). The tachyon Lagrangian is derived from the dynamics of a 3-brane moving in the five-dimensional bulk. The AdS5 geometry of the bulk is extended to include the radion. Using the Hamiltonian formalism we find four nonlinear field equations supplemented by the modified Friedmann equations of the RSII braneworld cosmology. After a suitable rescaling we reduce the parameters of our model to only one free parameter related to the brane tension and the AdS5 curvature. We solve the equations numerically assuming a reasonably wide range of initial conditions determined by physical considerations. Varying the free parameter and initial conditions we confront our results with the Planck 2015 data.


2016 ◽  
Vol 2016 ◽  
pp. 1-10 ◽  
Author(s):  
Z. Ossoulian ◽  
T. Golanbari ◽  
H. Sheikhahmadi ◽  
Kh. Saaidi

Using the noncanonical model of scalar field, the cosmological consequences of a pervasive, self-interacting, homogeneous, and rolling scalar field are studied. In this model, the scalar field potential is “nonlinear” and decreases in magnitude with increasing the value of the scalar field. A special solution of the nonlinear field equations ofϕthat has time dependency as fixed point is obtained. The fixed point relies on the noncanonical term of action andγ-parameter; this parameter appeared in energy density of scalar field redshift. By means of such fixed point the different eigenvalues of the equation of motion will be obtained. In different epochs in the evolution of the Universe for different values ofqandn, the potentials as a function of scalar field are attained. The behavior of baryonic perturbations in linear perturbation scenario as a considerable amount of energy density of scalar field at low redshifts prevents the growth of perturbations in the ordinary matter fluid. The energy density in the scalar field is not appreciably perturbed by nonrelativistic gravitational fields, in either the radiation or matter dominant or scalar field dominated epoch.


2012 ◽  
Vol 109 (26) ◽  
Author(s):  
Anton Peshkov ◽  
Igor S. Aranson ◽  
Eric Bertin ◽  
Hugues Chaté ◽  
Francesco Ginelli

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