Three-body relativistic flux tube model from QCD Wilson-loop approach

First we review the derivation of the relativistic flux tube model for a quark-antiquark system from Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration.\par A Hamiltonian can...

Descripción completa

Detalles Bibliográficos
Autores principales: Brambilla, N., Prosperi, G.M., Vairo, A.
Lenguaje:eng
Publicado: 1995
Materias:
Particle Physics - Phenomenology
Acceso en línea:https://dx.doi.org/10.1016/0370-2693(95)01170-U
http://cds.cern.ch/record/284789
_version_ 1780888194962685952
author Brambilla, N.
Prosperi, G.M.
Vairo, A.
author_facet Brambilla, N.
Prosperi, G.M.
Vairo, A.
author_sort Brambilla, N.
collection CERN
description First we review the derivation of the relativistic flux tube model for a quark-antiquark system from Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration.\par A Hamiltonian can be explicitly constructed as an expansion in 1 / m^2 or in the string tension \sigma. In the first case it reproduces the Wilson loop three-quark semirelativistic potential; in the second one, very complicated in general, but it reproduces known string models for slowly rotating quarks.
id cern-284789
institution Organización Europea para la Investigación Nuclear
language eng
publishDate 1995
record_format invenio
spelling cern-2847892023-02-27T03:51:35Zdoi:10.1016/0370-2693(95)01170-Uhttp://cds.cern.ch/record/284789engBrambilla, N.Prosperi, G.M.Vairo, A.Three-body relativistic flux tube model from QCD Wilson-loop approachParticle Physics - PhenomenologyFirst we review the derivation of the relativistic flux tube model for a quark-antiquark system from Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration.\par A Hamiltonian can be explicitly constructed as an expansion in 1 / m^2 or in the string tension \sigma. In the first case it reproduces the Wilson loop three-quark semirelativistic potential; in the second one, very complicated in general, but it reproduces known string models for slowly rotating quarks.First we review the derivation of the relativistic flux tube model for a quark-antiquark system from Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration.\par A Hamiltonian can be explicitly constructed as an expansion in $1 / m~2$ or in the string tension $\sigma$. In the first case it reproduces the Wilson loop three-quark semirelativistic potential; in the second one, very complicated in general, but it reproduces known string models for slowly rotating quarks.First we review the derivation of the relativistic flux tube model for a quark-antiquark system from Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration.\par A Hamiltonian can be explicitly constructed as an expansion in $1 / m~2$ or in the string tension $\sigma$. In the first case it reproduces the Wilson loop three-quark semirelativistic potential; in the second one, very complicated in general, but it reproduces known string models for slowly rotating quarks.First we review the derivation of the relativistic flux tube model for a quark-antiquark system from the Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration.First we review the derivation of the relativistic flux tube model for a quark-antiquark system from Wilson area law as we have given in a preceding paper. Then we extend the method to the three-quark case and obtain a Lagrangian corresponding to a star flux tube configuration. A Hamiltonian can be explicitly constructed as an expansion in $1 / m^2$ or in the string tension $\sigma$. In the first case it reproduces the Wilson loop three-quark semirelativistic potential; in the second one, very complicated in general, but it reproduces known string models for slowly rotating quarks.hep-ph/9507300CERN-TH-95-194IFUM-511-FTCERN-TH-95-194IFUM-511-FToai:cds.cern.ch:2847891995-07-13
spellingShingle Particle Physics - Phenomenology
Brambilla, N.
Prosperi, G.M.
Vairo, A.
Three-body relativistic flux tube model from QCD Wilson-loop approach
title Three-body relativistic flux tube model from QCD Wilson-loop approach
title_full Three-body relativistic flux tube model from QCD Wilson-loop approach
title_fullStr Three-body relativistic flux tube model from QCD Wilson-loop approach
title_full_unstemmed Three-body relativistic flux tube model from QCD Wilson-loop approach
title_short Three-body relativistic flux tube model from QCD Wilson-loop approach
title_sort three-body relativistic flux tube model from qcd wilson-loop approach
topic Particle Physics - Phenomenology
url https://dx.doi.org/10.1016/0370-2693(95)01170-U
http://cds.cern.ch/record/284789
work_keys_str_mv AT brambillan threebodyrelativisticfluxtubemodelfromqcdwilsonloopapproach
AT prosperigm threebodyrelativisticfluxtubemodelfromqcdwilsonloopapproach
AT vairoa threebodyrelativisticfluxtubemodelfromqcdwilsonloopapproach

Ejemplares similares