A Note on the evolution of cosmic string/superstring networks

Mairi Sakellariadou

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A Note on the evolution of cosmic string/superstring networks

Mairi Sakellariadou

High Energy Physics - Theory · Submitted 24 Oct 2004

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The cosmic superstring network has a scaling solution and the characteristic scale of the network is proportional to the square root of the reconnection probability.

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The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 2,290 input tokens, $0.0001 reported.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.05 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.17 · compares with prior results 0.07 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; show every role.

In the context of brane world scenario, cosmic superstrings can be formed in D-brane annihilation at the end of the brane inflationary era. The cosmic superstring network has a scaling solution and the characteristic scale of the network is proportional to the square root of the reconnection probability.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	In the context of brane world scenario, cosmic superstrings can be formed in D-brane annihilation at the end of the brane inflationary era.	background 0.99	0.09	0.07	asserted 0.79
s1	The cosmic superstring network has a scaling solution and the characteristic scale of the network is proportional to the square root of the reconnection probability.	result 0.98	0.47	0.57	asserted 1.00

What kind of paper the classifier reports this is: theoretical result 0.74 · evidence from argument 0.62.

What was examined, and what was not

sources read

arXiv listing abstract v2

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

In the context of brane world scenario, cosmic superstrings can be formed in D-brane annihilation at the end of the brane inflationary era. The cosmic superstring network has a scaling solution and the characteristic scale of the network is proportional to the square root of the reconnection probability.

Human review

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References

Forward citations

Cited by 12 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Cosmic superstrings in large volume compactifications: PTAs, LISA and time-varying tension
astro-ph.CO 2025-04 conditional novelty 7.0 of 10

Cosmic superstrings with a time-varying tension in large-volume string compactifications generically predict a LISA-band spectral drop and a high-frequency f^4 boost, encoding the mass and decay of the volume modulus.
Beyond the Standard Models with Cosmic Strings
hep-ph 2019-12 conditional novelty 6.0 of 10

Solving the velocity-dependent one-scale equations through cosmological transitions shifts the cosmic-string gravitational-wave turning point to lower frequency by a factor of about 22, letting future interferometers ...
Probing the gravitational wave background from cosmic strings with LISA
astro-ph.CO 2019-09 conditional novelty 6.0 of 10

LISA is projected to probe cosmic string tensions G mu down to about 1e-17 and to measure spectral features from early-universe physics.
Collisions of Cosmic F- and D-strings
hep-th 2004-05 accept novelty 6.0 of 10

Perturbative string calculations give reconnection probabilities for all pairs of cosmic F-, D-, and (p,q) strings, generally below one, so stringy cosmic strings can in principle be distinguished from gauge-theory solitons.
Cosmic string gravitational wave backgrounds at LISA: I. Signal survey, template reconstruction, and model comparison
astro-ph.CO 2025-08 unverdicted novelty 5.0 of 10

As provided, the manuscript body (random lasing) does not correspond to the abstract (cosmic string gravitational wave backgrounds at LISA), leaving the abstract's quantitative claims unsupported by any accessible text.

Show 7 more citing papers

What is the source of the PTA GW signal?
astro-ph.CO 2023-08 conditional novelty 5.0 of 10

A common-likelihood comparison of seven proposed sources of the nanohertz gravitational wave background finds that phase transitions, domain walls, scalar-induced and first-order gravitational waves fit the NANOGrav 1...
Comparison of cosmic string and superstring models to NANOGrav 12.5-year results
astro-ph.CO 2021-02 conditional novelty 5.0 of 10

Across four models of the gravitational-wave spectrum of cosmic string loops, the string tension that fits the NANOGrav 12.5-year common-spectrum signal stays in the range Gµ of roughly 10^-10.0 to 10^-10.7.
Gravitational radiation from cosmic (super)strings: bursts, stochastic background, and observational windows
hep-th 2004-10 conditional novelty 5.0 of 10

The gravitational wave bursts and stochastic background from cosmic string networks stay detectable by LIGO, LISA, and pulsar timing even when the reconnection probability is small and loop sizes are suppressed, with ...
Cosmological Backgrounds of Gravitational Waves and eLISA/NGO: Phase Transitions, Cosmic Strings and Other Sources
gr-qc 2012-01 conditional novelty 4.0 of 10

Refined gravitational-wave spectra from first-order phase transitions and cosmic string networks indicate that eLISA could detect phase transitions near 10 TeV and string tensions down to Gμ about 10^-13 for standard ...
Signals of Inflationary Models with Cosmic Strings
astro-ph.CO 2011-06 accept novelty 3.0 of 10

A review of the observational signatures of cosmic strings produced at the end of inflation, concluding that CMB data already bound the string tension G-mu below roughly 10^-6, while the loop population and hence the ...
Brane Inflation : String Theory viewed from the Cosmos
hep-th 2006-10 conditional novelty 3.0 of 10

Brane inflation in a warped flux compactification generically produces enough e-folds and leaves a scaling network of cosmic superstrings with tension between 10^-13 and 10^-6, testable by CMB, lensing, and gravitatio...
Introduction to Cosmic F- and D-Strings
hep-th 2004-12 accept novelty 3.0 of 10

Cosmic-scale F- and D-strings can arise naturally when branes annihilate at the end of warped brane inflation, and their gravitational-wave cusps could be detectable by LIGO.

How the literature uses it

31 arXiv papers cite this in 46 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 28 sentences without a confident label

Uses its data or values 1 paper

Numerical studies [ref] suggest values between $-1$ and $-0.6$ for the exponent.

Analytic Approaches to the Study of Small Scale Structure on Cosmic String Networks · Summary and discussion · 0.87

Compares with it 3 papers

Our result of $ρ_∞∝P_eff^-1$ is consistent with the one obtained in Ref. [ref] .

Cosmic strings from pure Yang-Mills theory · Extended VOS model · 0.96
The VOS predicts $β=0$ (since the increase of small scale structure generates a new scale that is not present in the model, see [ref] ), whilst simulations indicate $β=1/2$ in flat space [ref] and $β=2/3$ in an expanding spacetime [ref] .

Cosmic superstrings in large volume compactifications: PTAs, LISA and time-varying tension · The VOS model (with a time dependent tension) · 0.83
This $P$ dependence is consistent with the numerical simulations in [ref] , while [ref] obtained a relatively weaker dependence, $ρ_str∝P^-α$ with $0 < α< 1$.

Weak lensing of CMB by cosmic (super-)strings · String network dynamics · 0.97

Cites it as support 1 paper

It can thus be much less than one, leading to an increased density of strings [ref] , implying an enhancement of various observational signatures.

Cosmic Strings and Cosmic Superstrings · Differences between Cosmic Strings and Cosmic Superstrings · 0.97

Cites it as background 12 papers

In 4-dimensional spacetime, $A_μν$ is dual to an axion $a$ i.e. $∂^μa=ϵ^μνρσ∂_νA_ρσ$.[A realistic compactification from 10 to 4 dimensions in Type IIB string theory possesses an orientifold, in which the original two-forms $B_μν$ and $C_μν$ are projected out [ref] .

Periodic Fast Radio Bursts from Axion Emission by Cosmic Superstrings · Introduction · 0.91
In a number of studies, cosmic superstring evolution has been addressed via numerical experiments [ref] .

Dynamics of F/D networks: the role of bound states · Introduction · 0.95
The reader can find in the literature a number of numerical experiments [ref] with cosmic superstrings, each of them at a different level of approximation, as well as analytical studies [ref] .

Numerical experiments with p F- and q D-strings: the formation of (p,q) bound states · Introduction · 0.99

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