scholarly journals Phantom field withO(N)symmetry in an exponential potential

2004 ◽  
Vol 69 (10) ◽  
Author(s):  
Xin-zhou Li ◽  
Jian-gang Hao
Keyword(s):  
Exponential Potential ◽  
Phantom Field

Dirac equation with multiparameter-potential and Hulthén tensor interaction under relativistic symmetries

Open Physics ◽  
2014 ◽  
Vol 12 (12) ◽  
Author(s):  
Sami Ortakaya
Keyword(s):  
Dirac Equation ◽  
Spin Symmetry ◽  
Tensor Interaction ◽  
Numerical Results ◽  
Exponential Potential ◽  
Energy Eigenvalues ◽  
Nu Method

AbstractThe pseudospin and spin symmetric solutions of the Dirac equation with Hulthén-type tensor interaction are obtained under multi-parameter-exponential potential (MEP) for arbitrary κ states. The energy eigenvalues and the corresponding eigenfunctions are also obtained using the parametric Nikiforov-Uvarov (NU) method. Some numerical results are also obtained for pseudospin and spin symmetry limits.

Estimating the error in variational scattering calculations

1978 ◽  
Vol 56 (10) ◽  
pp. 1358-1364 ◽  
Author(s):  
J. W. Darewych ◽  
R. Pooran
Keyword(s):  
Wave Scattering ◽  
Exponential Potential ◽  
S Wave ◽  
Order Error ◽  
Absolute Value ◽  
First Order ◽  
Scattering Phase ◽  
Square Well ◽  
Scattering Phase Shifts ◽  
Made In

We derive bounds to the absolute value of the error that is made in variational estimates of scattering phase shifts. These bounds, like the variational estimates, are second order in 'small' quantities and are, in this respect, an improvement on similar but first-order error bounds derived previously by Bardsley, Gerjuoy, and Sukumar. The s-wave scattering by a square well potential, in the Born approximation, and by an exponential potential, using a many parameter trial function, are used to illustrate the results.

scholarly journals Autonomous dynamical system description of de Sitter evolution in scalar assisted f(R) − ϕ gravity

2018 ◽  
Vol 15 (12) ◽  
pp. 1850212 ◽  
Author(s):  
K. Kleidis ◽  
V. K. Oikonomou
Keyword(s):  
Dynamical System ◽  
Numerical Analysis ◽  
Scalar Field ◽  
Analysis Approach ◽  
Single Variable ◽  
De Sitter ◽  
Exponential Potential ◽  
System Description ◽  
Variable Formula ◽  
Autonomous Dynamical System

In this paper we will study the cosmological dynamical system of an [Formula: see text] gravity in the presence of a canonical scalar field [Formula: see text] with an exponential potential by constructing the dynamical system in a way that it is rendered autonomous. This feature is controlled by a single variable [Formula: see text], which when it is constant, the dynamical system is autonomous. We focus on the [Formula: see text] case which, as we demonstrate by using a numerical analysis approach, leads to an unstable de Sitter attractor, which occurs after [Formula: see text] [Formula: see text]-foldings. This instability can be viewed as a graceful exit from inflation, which is inherent to the dynamics of de Sitter attractors.

Solutions of the Two-Body Salpeter Equation Under an Exponential Potential for Any l State

2011 ◽  
Vol 52 (1-2) ◽  
pp. 165-170 ◽  
Author(s):  
S. Zarrinkamar ◽  
A. A. Rajabi ◽  
H. Hassanabadi
Keyword(s):  
Exponential Potential

scholarly journals A double exponential potential for van der Waals interaction

AIP Advances ◽  
2019 ◽  
Vol 9 (6) ◽  
pp. 065304 ◽  
Author(s):  
Xiongwu Wu ◽  
Bernard R. Brooks
Keyword(s):  
Van Der Waals ◽  
Van Der Waals Interaction ◽  
Exponential Potential ◽  
Double Exponential

scholarly journals Tachyonic matter cosmology with exponential and hyperbolic potentials

2017 ◽  
Vol 26 (02) ◽  
pp. 1750012 ◽  
Author(s):  
B. Pourhassan ◽  
J. Naji
Keyword(s):  
Scalar Field ◽  
Observational Data ◽  
Cosmological Parameters ◽  
Field Potentials ◽  
Exponential Potential ◽  
Frw Universe ◽  
Hyperbolic Cosine ◽  
Special Cases ◽  
Friedmann Robertson Walker ◽  
Type Potential

In this paper, we consider tachyonic matter in spatially flat Friedmann–Robertson–Walker (FRW) universe, and obtain behavior of some important cosmological parameters for two special cases of potentials. First, we assume the exponential potential and then consider hyperbolic cosine type potential. In both cases, we obtain behavior of the Hubble, deceleration and EoS parameters. Comparison with observational data suggest the model with hyperbolic cosine type scalar field potentials has good model to describe universe.

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