Extending the velocity-dependent one-scale string evolution model

By C. Martins, E. Shellard. 2000

200 citations recorded by the source corpus.

We provide a general overview of the velocity-dependent one-scale model for cosmic string evolution and discuss two further extensions to it. We introduce and justify a new ansatz for the momentum parameter k, and also incorporate the effect of radiation back reaction. We thus discuss the evolution of the basic large-scale features of cosmic string networks in all relevant cosmological scenarios, concentrating in particular on the ``scaling'' solutions relevant for each case. In a companion paper, we show, by comparing with numerical simulations, that this model provides an accurate description of the large-scale features of cosmic string networks.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/300d13b982eba6d378f771a8a9553468e9d1cd04

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Marek Lewicki
2. G. Servant
3. W. Buchmuller
4. Daniel G. Figueroa
5. P. Simakachorn
6. Y. Gouttenoire
7. Yanou Cui
8. J. Wells

In Nuclear and High Energy Physics

1. G. Servant
2. Marek Lewicki
3. P. Simakachorn
4. Y. Gouttenoire
5. E. Nardi
6. Daniel G. Figueroa
7. W. Buchmuller
8. Yanou Cui

Citations in the corpus

• From NANOGrav to LIGO with metastable cosmic strings (2020, methodology): “1, the analysis in [16] employs the analytical velocity-dependent onescale (VOS) model [30–32] instead of the BOS model.”
• Probing the pre-BBN universe with gravitational waves from cosmic strings (2018, methodology): “ c] 2(n 2) ; v = s n 2 k(v) [k(v) + c] 1 2 n ; (2.3) where cis a loop chopping eciency parameter and k(v) is a function of vto be determined. We x c= 0:23 based on numerical simulations [94], and we use the ansatz of Ref. [94] for { 4 { the function k(v): k(v) = 2 p 2 ˇ p 1 v2 1 + 2 2v3 1 8v6 1 +”
• The landscape of QCD axion models (2020, methodology): “A more accurate description is obtained by accounting for the effects of the velocity of the centre of mass of the string [223–225].”
• Probing the gravitational wave background from cosmic strings with LISA (2019, methodology): “4 In terms of the characteristic length L ≡ (μ/ρ∞) — which measures the average distance between long strings — and v̄, the VOS equations of motion are [119, 120]”
• TASI Lectures on the Strong CP Problem and Axions (2018, background): “The expectation is that approximately O(1) number of strings is left in each Hubble volume at all times [100, 101, 102, 103, 104, 105, 106].”
• Beyond the Standard Models with cosmic strings (2019, methodology): “xtended) AH (c = 0.57) T eq Figure 25: Left: GW spectra with dierent VOS modellings of the long-string network evolution. The VOS models are either based on NG simulations (solid line - ~c = 0:23) [175] or abelian-Higgs (AH) eld theory simulations (dashed line - ~c= 0:57) [132,221], possibly extend”