Type I Abelian Higgs strings: evolution and Cosmic Microwave Background constraints - INSPIRE

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Type I Abelian Higgs strings: evolution and Cosmic Microwave Background constraints

Mark Hindmarsh
(
- Sussex U. and
- Helsinki Inst. of Phys.
)
,
Joanes Lizarraga
(
- Basque U., Bilbao
)
,
Jon Urrestilla
(
- Basque U., Bilbao
)
,
David Daverio
(
- Cambridge U., DAMTP
)
,
Martin Kunz
(
- Geneva U.
)

Dec 20, 2018

12 pages

Published in:

Phys.Rev.D 99 (2019) 8, 083522

Published: Apr 27, 2019

e-Print:

1812.08649 [astro-ph.CO]

DOI:

10.1103/PhysRevD.99.083522

View in:

reference search23 citations

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Abstract: (APS)

We present results from the first simulations of networks of Type I Abelian Higgs cosmic strings to include both matter and radiation eras and cosmic microwave background (CMB) constraints. In Type I strings, the string tension is a slowly decreasing function of the ratio of the scalar and gauge mass-squared, β. We find that the mean string separation shows no dependence on β, and that the energy-momentum tensor correlators decrease approximately in proportion to the square of the string tension, with additional O(1) correction factors which asymptote to constants below β≲0.01. Strings in models with low self-couplings can therefore satisfy current CMB bounds at higher symmetry-breaking scales. This is particularly relevant for models where the gauge symmetry is broken in a supersymmetric flat direction, for which the effective self-coupling can be extremely small. If our results can be extrapolated to β≃10-15, even strings formed at 1016 GeV (approximately the grand unification scale in supersymmetric extensions of the Standard Model) can be compatible with CMB constraints.

Note:

11 pages, 9 figures. v2 Discussion of previous Type I cosmic string simulations added (Ref. [36]), main results unchanged. v3 matches published version

Cosmology
supersymmetry: flat direction
scale: grand unified theory
symmetry breaking: scale
tensor: energy-momentum
symmetry: gauge
cosmic background radiation
string
string tension
abelian

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