Introduction

Graham, Noah; Quandt, Markus; Weigel, H.

doi:10.1007/978-3-642-00139-0_1

Cited by 16 publications

(18 citation statements)

References 24 publications

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“…We have developed a procedure to compute the VPE of cosmic strings with spectral methods [12]. We have verified this procedure numerically by reproducing the required invariances even though the individual entries of the calculation are not invariant by themselves.…”

Section: Discussionmentioning

confidence: 99%

Cosmic Strings Stabilized by Quantum Fluctuations

Weigel

2017

Russ Phys J

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We compute fermion quantum corrections to the energy of cosmic strings. A number of rather technical tools is needed to formulate this correction and we employ isospin and gauge invariance to verify consistency of these tools. These corrections must also be included when computing the energy of strings that are charged by populating fermion bound states in its background. We find that charged strings are dynamically stabilized in theories similar to the standard model of particle physics.

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Section: Discussionmentioning

confidence: 99%

Cosmic Strings Stabilized by Quantum Fluctuations

Weigel

2017

Russ Phys J

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“…First, spectral methods are employed to express this energy in form of scattering data 23 . The equivalence of terms in the Born series and Feynman diagrams makes it possible to impose standard renormalization conditions.…”

Section: Formalismmentioning

confidence: 99%

Cosmic Strings Stabilized by Fermion Fluctuations

Weigel

Quandt

Graham

2012

Int. J. Mod. Phys. Conf. Ser.

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We provide a thorough exposition of recent results on the quantum stabilization of cosmic strings. Stabilization occurs through the coupling to a heavy fermion doublet in a reduced version of the standard model. The study combines the vacuum polarization energy of fermion zero-point fluctuations and the binding energy of occupied energy levels, which are of the same order in a semi-classical expansion. Populating these bound states assigns a charge to the string. Strings carrying fermion charge become stable if the Higgs and gauge fields are coupled to a fermion that is less than twice as heavy as the top quark. The vacuum remains stable in the model, because neutral strings are not energetically favored. These findings suggest that extraordinarily large fermion masses or unrealistic couplings are not required to bind a cosmic string in the standard model.

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“…In situations where the number of external degrees of freedom or quantum numbers is large, the leading corrections come from the small amplitude fluctuations, which can be efficiently computed using spectral methods [35], at least when there is sufficient symmetry to formulate a scattering problem. Formally, this correction is of order O( ).…”

Section: A Quantum Action For the Instable Modementioning

confidence: 99%

“…The study of a toroidal string configuration is significantly more complicated than that of an infinitely long and axially symmetric string because the field equations cannot be simplified to ordinary differential equations of a single variable. This hampers the application of spectral methods, which have previously been used successfully to compute quantum effects for localized field configurations [35]. We will therefore adopt a different technique that has proven successful in describing similar quantum mechanical scenarios.…”

Section: Introductionmentioning

confidence: 99%