A new parallel simulation technique

Benjamin Shlaer; Jose J. Blanco-Pillado; Ken D. Olum

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A new parallel simulation technique

Jose J. Blanco-Pillado, Ken D. Olum, Benjamin Shlaer

Computational Physics · Submitted 17 Nov 2010

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

The authors' main claim We compare a cosmic string simulation we developed using the semi-parallel technique with our previous MPI-based code for several test cases and find a factor of 2.6 improvement in the total amount of processor time required to accomplish the same job for strings evolving in the matter-dominated era.

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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, 4,296 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.17 · human participants 0.01 · controlled comparison 0.83 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.98 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

We develop a "semi-parallel" simulation technique suggested by Pretorius and Lehner, in which the simulation spacetime volume is divided into a large number of small 4-volumes which have only initial and final surfaces. Thus there is no two-way communication between processors, and the 4-volumes can be simulated independently without the use of MPI. This technique allows us to simulate much larger volumes than we otherwise could, because we are not limited by total memory size. No processor time is lost waiting for other processors. We compare a cosmic string simulation we developed using the semi-parallel technique with our previous MPI-based code for several test cases and find a factor of 2.6 improvement in the total amount of processor time required to accomplish the same job for strings evolving in the matter-dominated era.

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	We develop a "semi-parallel" simulation technique suggested by Pretorius and Lehner, in which the simulation spacetime volume is divided into a large number of small 4-volumes which have only initial and final surfaces.	method 0.70	0.79	0.08	asserted 1.00
s1	Thus there is no two-way communication between processors, and the 4-volumes can be simulated independently without the use of MPI.	method 0.99	0.49	0.08	asserted 1.00
s2	This technique allows us to simulate much larger volumes than we otherwise could, because we are not limited by total memory size.	interpretation 0.49	0.71	0.18	asserted 0.96
s3	No processor time is lost waiting for other processors.	interpretation 0.37	0.56	0.08	asserted 1.00
s4	We compare a cosmic string simulation we developed using the semi-parallel technique with our previous MPI-based code for several test cases and find a factor of 2.6 improvement in the total amount of processor time required to accomplish the same job for strings evolving in the matter-dominated era.	result 1.00	0.97	0.60	asserted 1.00

What kind of paper the classifier reports this is: method or tool 1.00 · evidence from simulation or computation 1.00.

What was examined, and what was not

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arXiv listing abstract v1

not examined

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

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P abstract

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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

We develop a "semi-parallel" simulation technique suggested by Pretorius and Lehner, in which the simulation spacetime volume is divided into a large number of small 4-volumes which have only initial and final surfaces. Thus there is no two-way communication between processors, and the 4-volumes can be simulated independently without the use of MPI. This technique allows us to simulate much larger volumes than we otherwise could, because we are not limited by total memory size. No processor time is lost waiting for other processors. We compare a cosmic string simulation we developed using the semi-parallel technique with our previous MPI-based code for several test cases and find a factor of 2.6 improvement in the total amount of processor time required to accomplish the same job for strings evolving in the matter-dominated era.

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References

Forward citations

Cited by 2 Pith papers

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

The number of cosmic string loops
astro-ph.CO 2013-09 conditional novelty 6.0 of 10

The paper derives the mass and velocity distribution of cosmic string loops from simulations and converts it into a pulsar-timing bound on the string tension of Gμ ≤ 2.8×10⁻⁹.
Large parallel cosmic string simulations: New results on loop production
astro-ph.CO 2011-01 conditional novelty 5.0 of 10

Cosmic string simulations with roughly ten times the previous dynamic range show a scaling population of loops at about one twentieth the horizon size emerging from beneath a long-lived transient of small loops.

How the literature uses it

5 arXiv papers cite this in 8 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 · 4 sentences without a confident label

Uses its method or tool 3 papers

For details on the simulation procedure see Refs. [ref] .

The number of cosmic string loops · Radiation era · 0.87
We have developed a new parallel computing technique [ref] that has allowed us to run the largest cosmic string simulations ever performed, reaching an increase in dynamic range of roughly an order of magnitude with respect to previous studies.

Large parallel cosmic string simulations: New results on loop production · Conclusions · 0.91
Our simulation process is described in detail in Refs. [ref] .

Cosmic string loop shapes · Loops at formation · 0.90

What it cites · 14 sentences without a confident label

Uses the method or tool of 4 papers

For details on the algorithm see [ref] .

Scaling of cosmic string loops · Semi-parallel cosmic string simulation · 0.84
For details on the algorithm see [ref] .

Cosmic string loops in the expanding universe · Semi-parallel cosmic string simulation · 0.84
For details on the algorithm see [ref] .

Cosmic string scaling in flat space · Semi-parallel cosmic string simulation · 0.84

Compares with 1 paper

For comparison, the Millennium Simulation [ref] used just over 10 billion particles.

Simulating the joint evolution of quasars, galaxies and their large-scale distribution · Results · 0.91

Cites as background 3 papers

Cosmic strings are astrophysically long, microphysically thin objects which may have been formed early in the universe through a phase transition [ref] or at the end of inflation driven by superstring theory [ref] .

Formation and evolution of cosmic D-strings · Semi-parallel cosmic string simulation · 0.99
Cosmic strings are astrophysically long, microphysically thin objects which may have been formed early in the universe through a phase transition [ref] or at the end of inflation driven by superstring theory [ref] .

Cosmic String Production Towards the End of Brane Inflation · Semi-parallel cosmic string simulation · 0.99
Cosmic strings are astrophysically long, microphysically thin objects which may have been formed early in the universe through a phase transition [ref] or at the end of inflation driven by superstring theory [ref] .

Cosmic F- and D-strings · Semi-parallel cosmic string simulation · 0.99

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