Equations Of Relativistic String Research Articles

A Globally Smooth Solution to the Relativistic String Equation

A Globally Smooth Solution to the Relativistic String Equation

Riemann problem and wave interactions for the one-dimensional relativistic string equation in Minkowski space

In this paper, we consider the Riemann problem for the one-dimensional relativistic string equation in Minkowski space. It is shown that the delta shock wave will be constructed in the Riemann solutions in some certain situations. Furthermore, the interactions of elementary waves including contact discontinuity and delta shock wave are obtained.

Stability of traveling wave for the relativistic string equation in de Sitter spacetime

In this paper, we are concerned with the relativistic string equations in de Sitter spacetime. Since the background spacetime is nonflat, the governing system of equations is semilinear under the usual isothermal coordinates, contrary to the linear wave equations in the Minkowski spacetime. Based on the null condition enjoyed by the system and the method of [Luli et al., Adv. Math 329, 174–188 (2018)], we succeeded in proving the stability of the traveling wave solution to the relativistic string equations. We note that the traveling wave solution should be small in the sense of weighted energy.

Comment on “Stationary rotating strings as relativistic particle mechanics”

The set of rigidly rotating solutions to the relativistic string equation with subluminal azimuthal velocity has recently been reported by Ogawa et al. This set, together with a second set of rigidly rotating strings with superluminal azimuthal velocity, was reported in earlier papers by Burden and Tassie, and independently by Embacher. We believe the second set is also physically relevant to modelling cosmic strings. We write both sets of rigidly rotating string solutions in the aligned standard gauge and give a geometrical interpretation.

Integrals of periodic motion for classical equations of relativistic string with masses at ends

Boundary equations for the relativistic string with masses at ends are formulated in terms of geometrical invariants of world trajectories of masses at the string ends. In the three-dimensional Minkowski space , there are two invariants of that sort, the curvature K and torsion . Curvatures of trajectories of the string massive ends are always constant, , whereas torsions are the functions of and obey a system of differential equations of second order with deviating arguments. For periodic torsions , where l is the string length in the plane of parameters and , these equations result in constant of motion.

Additional Rigidly Rotating Solutions in the String Model of Hadrons

Solutions to the relativistic string equation are found which correspond to rigid body rotation about the z-axis with azimuthal velocity greater than the velocity of light. If the solutions lie entirely in the x-y plane they are rotating epicycloids, complimentary to the hypocycloid solutions found previously. The use of a general solution to the string equation in terms of two arbitrary world-lines with null tangents provides an alternative derivation of the rigidly rotating solutions.

Some exotic mesons and glueballs from the string model

Planar solutions are found to the relativistic string equation corresponding to rigid-body rotation. These solutions allow for the construction of certain classes of exotic mesons and of glueballs with asymptotically straight Chew-Frautschi plots. We determine the asymptotic slope of the Chew-Frautschi plots for these hadrons.

Rotating Strings, Glueballs and Exotic Mesons

The relativistic string equation is solved for motion corresponding to rigid body rotation about the z-axis. One class of these solutions, namely the planar solutions, allows for the construction of two types of exotic meson and one type of glueball, all of which have asymptotically straight ChewFrautschi plots. The first type of meson only exists when the number of quarks or antiquarks is 4, 5, 6 or 7, whereas no such restriction applies to the second type. For each of these cases the first type of meson is energetically more favourable than the second type for a given angular momentum.