Solving relativistic bound-state problems in a self-interacting complex scalar field model by discretized light-cone quantization in 1 + 1 dimensions

1994 ◽  
Vol 49 (6) ◽  
pp. 2997-3002 ◽  
Author(s):  
S. N. Ghosh
Keyword(s):  
Scalar Field ◽  
Light Cone ◽  
Field Model ◽  
Bound State ◽  
Complex Scalar ◽  
Scalar Field Model ◽  
Complex Scalar Field ◽  
Light Cone Quantization

The classical and quantum cosmology with a complex scalar field

1992 ◽  
Vol 169 (4) ◽  
pp. 308-312 ◽  
Author(s):  
I.M. Khalatnikov ◽  
A. Mezhlumian
Keyword(s):  
Scalar Field ◽  
Quantum Cosmology ◽  
Complex Scalar ◽  
Complex Scalar Field

Self-interacting complex scalar field as dark matter

2011 ◽  
Author(s):  
F. Briscese ◽  
Luis Arturo Ureña-López ◽  
Hugo Aurelio Morales-Técotl ◽  
Román Linares-Romero ◽  
Elí Santos-Rodríguez ◽  
...  
Keyword(s):  
Dark Matter ◽  
Scalar Field ◽  
Complex Scalar ◽  
Complex Scalar Field

scholarly journals Hadamard parametrix of the Feynman Green’s function of a five-dimensional charged scalar field

2020 ◽  
Vol 29 (11) ◽  
pp. 2041002
Author(s):  
Visakan Balakumar ◽  
Elizabeth Winstanley
Keyword(s):  
Scalar Field ◽  
Green’S Function ◽  
Green's Function ◽  
Minkowski Spacetime ◽  
Energy Tensor ◽  
Complex Scalar ◽  
Charged Scalar ◽  
Taylor Series Expansions ◽  
Complex Scalar Field ◽  
Charged Scalar Field

The Hadamard parametrix is a representation of the short-distance singularity structure of the Feynman Green’s function for a quantum field on a curved spacetime background. Subtracting these divergent terms regularizes the Feynman Green’s function and enables the computation of renormalized expectation values of observables. We study the Hadamard parametrix for a charged, massive, complex scalar field in five spacetime dimensions. Even in Minkowski spacetime, it is not possible to write the Feynman Green’s function for a charged scalar field exactly in closed form. We, therefore, present covariant Taylor series expansions for the biscalars arising in the Hadamard parametrix. On a general spacetime background, we explicitly state the expansion coefficients up to the order required for the computation of the renormalized scalar field current. These coefficients become increasingly lengthy as the order of the expansion increases, so we give the higher-order terms required for the calculation of the renormalized stress-energy tensor in Minkowski spacetime only.

Sign in / Sign up

Export Citation Format

Share Document