The dynamical interactions of cosmic strings

Moriarty, K.J.M.; Myers, Eric; Rebbi, C.

doi:10.1016/0021-9991(90)90189-8

Cited by 13 publications

(14 citation statements)

References 10 publications

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“…But instead abelian cosmic strings always intercommute upon colliding. [27,28,29] Intercommuting reduces the amount of infinite string per unit co-moving volume by allowing loops to be chopped off and by preventing infinite strings from becoming straightened out and stretched. Causality prevents the density of infinite strings from dropping below approximately one infinite string per horizon volume.…”

Section: Semilocal Strings and Cosmologymentioning

confidence: 99%

Skyrmions and semilocal strings in cosmology

Benson

Bucher²

1993

Nuclear Physics B

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It has been pointed out that cosmic string solutions can exist in gauge field theories with broken symmetry even when π 1 (G/H) is trivial. The stability of such semilocal defects is not guaranteed by topology and depends on dynamical considerations. In the literature it has been tacitly assumed that if stable, such strings would form in the Early Universe in a manner analogous to the formation of a network of more robust topologically-stable strings. In this paper we find that except for unnaturally small values of the correlation length, a network of semilocal strings does not form. Instead, delocalized skyrmionic string configurations, which expand with the Hubble flow, dominate.

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Section: Semilocal Strings and Cosmologymentioning

confidence: 99%

Skyrmions and semilocal strings in cosmology

Benson

Bucher²

1993

Nuclear Physics B

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“…To describe the collision of the angled D-strings, we turn on a small relative velocity v(> 0), 8) as in (2.2). For very small velocity, the fluctuation analysis in the previous subsection is valid (v ≪ θ ≪ 1).…”

Section: Time Evolution Of Tachyon Wave Function and Reconnection Conmentioning

confidence: 99%

“…This reconnection probability is one of the indispensable ingredients for simulating galaxy formation in the early universe, and is important also for the direct detection of gravitational waves arising from cusps created when the cosmic strings are reconnected. For the vortex strings, numerical simulations [6,7,8] have been extensively performed and exhibit the universal feature: these vortex strings always reconnect classically for small collision velocities, while above a velocity upper bound they do not reconnect. On the other hand, for fundamental strings and D-strings, the reconnection is probabilistic for any collision velocity [9].…”

Section: Introductionmentioning

confidence: 99%

Reconnection of colliding cosmic strings

Hanany¹,

Hashimoto²

2005

J. High Energy Phys.

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For vortex strings in the Abelian Higgs model and D-strings in superstring theory, both of which can be regarded as cosmic strings, we give analytical study of reconnection (recombination, inter-commutation) when they collide, by using effective field theories on the strings. First, for the vortex strings, via a string sigma model, we verify analytically that the reconnection is classically inevitable for small collision velocity and small relative angle. Evolution of the shape of the reconnected strings provides an upper bound on the collision velocity in order for the reconnection to occur. These analytical results are in agreement with previous numerical results. On the other hand, reconnection of the D-strings is not classical but probabilistic. We show that a quantum calculation of the reconnection probability using a D-string action reproduces the nonperturbative nature of the worldsheet results by Jackson, Jones and Polchinski. The difference on the reconnection -classically inevitable for the vortex strings while quantum mechanical for the D-strings -is suggested to originate from the difference between the effective field theories on the strings.

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“…Numerical studies of vortex scattering are just becoming possible, and tend to confirm the geodesic picture. 8 The remainder of this Letter is concerned with soliton dynamics when the static forces are weak but nonzero. One may again define a reduced finite-dimensional dynamics.…”

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confidence: 99%

Unstable Manifolds and Soliton Dynamics

Manton

1988

Phys. Rev. Lett.

108

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It is argued that the interactions between solitons are well approximated by a finite-dimensional dynamical system, provided that the static forces between the solitons are relatively weak. The application to skyrmion dynamics and the nucleon-nucleon interaction is described.PACS numbers: 1 l. lO.Lm, 02.40.+m, 13.75.Cs This Letter is concerned with the truncation of a Lagrangean field theory to a finite-dimensional Lagrangean dynamical system. Most classical field theories, and all those considered here, are based on an infinite-dimensional configuration space G, the space of field configurations at a particular time, on which is defined a metric and a potential energy function V. From the metric one obtains the kinetic energy T as an infinite-dimensional version of jgijV l v J . The Lagrangean of the theory is T -V. Lorentz invariance implies that the functional forms of T and V are related, but this will not concern us. A truncation of the theory is defined as the Lagrangean dynamics on a submanifold M of G, with the induced metric and potential energy function. In general, the solutions of the equations of motion on M will not correspond to solutions of the original field equations, because the original theory has no forces constraining the motion to M. In some circumstances, however, there are effective constraining forces, and the full field dynamics does approximately reduce to motion on a suitable finite-dimensional manifold M. Such a truncation is particularly useful in theories with solitons-meaning vortices, monopoles, skyrmions, etc., rather than the solitons in exactly integrable theories. An approximate quantization is possible with Hamiltonian -V 2 +F, where V 2 is the covariant Laplacian on M and V the induced potential.In the dynamics of single solitons one usually makes a finite-dimensional truncation of the infinite-dimensional field dynamics. A single soliton configuration is never unique and is labeled by collective coordinates which include position coordinates, and often internal coordinates as well. These collective coordinates parametrize a manifold M which is an orbit of the symmetry group of the theory. The metric on M is invariant under the group action and depends on the mass and moments of inertia of the soliton, and also on moments associated with internal symmetries. The potential energy of M is a constant, equal to the mass of the soliton, so the Lagrangean on M has essentially just a kinetic term coming from the metric. The dynamics on M is therefore geodesic motion at constant speed. This accurately describes the classical motion of a free soliton provided all speeds are small. The geodesic dynamics gives non-Abelian monopoles spatial momentum and electric charge. It gives skyrmions a correlated angular momentum and isospin as well as spatial momentum. The geodesic dynamics is only an approximation, as it ignores Lorentz contraction and the centrifugal deformation of the soliton due to internal motion.A second situation where one can truncate the field theory is in the low-ene...

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The dynamical interactions of cosmic strings

Cited by 13 publications

References 10 publications

Skyrmions and semilocal strings in cosmology

Skyrmions and semilocal strings in cosmology

Reconnection of colliding cosmic strings

Unstable Manifolds and Soliton Dynamics

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