Abstract
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. A Hamiltonian can be explicitly constructed as an expansion in 1 m2 or in the string tension σ. In the first case it reproduces the Wilson loop three-quark semirelativistic potential; in the second one, it is very complicated in general, but it reproduces known string models for slowly rotating quarks.
Original language | English |
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Pages (from-to) | 113-122 |
Number of pages | 10 |
Journal | Physics Letters B |
Volume | 362 |
Issue number | 1-4 |
DOIs | |
State | Published - 9 Nov 1995 |
Externally published | Yes |