A formalism for the construction of binary neutron stars with arbitrary circulation

Stuart L. Shapiro; Thomas W. Baumgarte

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A formalism for the construction of binary neutron stars with arbitrary circulation

General Relativity and Quantum Cosmology · Submitted 4 Sep 2009

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

The authors' main claim In this paper we develop a new formalism for the construction of binary stars with circulation intermediate between corotational and irrotational.

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arXiv ID0909.0952 (version 2)

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CitationStuart L. Shapiro, Thomas W. Baumgarte. "A formalism for the construction of binary neutron stars with arbitrary circulation." arXiv:0909.0952 (2009). https://pith.science/paper/R5QWRMLL

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What the abstract itself states, as probabilities: claims first 0.10 · states limitation 0.09 · human participants 0.01 · controlled comparison 0.06 · randomized assignment 0.01 · states quantitative result 0.03 · compares with prior results 0.66 · mentions code or data availability 0.02.

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Most numerical models of binary stars - in particular neutron stars in compact binaries - assume the companions to be either corotational or irrotational. Either one of these assumptions leads to a significant simplification in the hydrodynamic equations of stationary equilibrium. In this paper we develop a new formalism for the construction of binary stars with circulation intermediate between corotational and irrotational. Generalizing the equations for irrotational flow we cast the Euler equation, which is an algebraic equation in the case of corotational or irrotational fluid flow, as an elliptic equation for a new auxiliary quantity. We also suggest a parameterized decomposition of the fluid flow that allows for a variation of the stellar circulation.

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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	Most numerical models of binary stars - in particular neutron stars in compact binaries - assume the companions to be either corotational or irrotational.	background 0.99	0.04	0.02	asserted 1.00
s1	Either one of these assumptions leads to a significant simplification in the hydrodynamic equations of stationary equilibrium.	background 0.98	0.08	0.03	asserted 1.00
s2	In this paper we develop a new formalism for the construction of binary stars with circulation intermediate between corotational and irrotational.	contribution 1.00	0.96	0.39	asserted 1.00
s3	Generalizing the equations for irrotational flow we cast the Euler equation, which is an algebraic equation in the case of corotational or irrotational fluid flow, as an elliptic equation for a new auxiliary quantity.	method 0.93	0.91	0.14	asserted 1.00
s4	We also suggest a parameterized decomposition of the fluid flow that allows for a variation of the stellar circulation.	method 0.68	0.91	0.10	hedged possibility 0.98

What kind of paper the classifier reports this is: method or tool 0.98 · evidence from proof or derivation 1.00.

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The paper

Original abstract

Most numerical models of binary stars - in particular neutron stars in compact binaries - assume the companions to be either corotational or irrotational. Either one of these assumptions leads to a significant simplification in the hydrodynamic equations of stationary equilibrium. In this paper we develop a new formalism for the construction of binary stars with circulation intermediate between corotational and irrotational. Generalizing the equations for irrotational flow we cast the Euler equation, which is an algebraic equation in the case of corotational or irrotational fluid flow, as an elliptic equation for a new auxiliary quantity. We also suggest a parameterized decomposition of the fluid flow that allows for a variation of the stellar circulation.

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References

Forward citations

Cited by 4 Pith papers

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

Mergers of binary neutron stars with realistic spin
gr-qc 2013-11 conditional novelty 6.0 of 10

Evolving binary neutron stars with realistic aligned or anti-aligned spin through the last three orbits shows spin-orbit coupling shifts the merger phase by up to 0.7 gravitational-wave cycles and lowers the remnant's...
A comprehensive simulation framework for multi-modal kilonova observations from all-sky surveys
astro-ph.IM 2026-10 conditional novelty 5.0 of 10

A multimodal kilonova simulation pipeline produces survey-realistic light curves, spectra, and image pairs intended for training AI classifiers and parameter estimators.
Gravitational waves from neutron star mergers and their relation to the nuclear equation of state
astro-ph.HE 2019-07 accept novelty 2.0 of 10

A review arguing that gravitational-wave observations of neutron-star mergers, especially GW170817, already constrain the supranuclear equation of state, favoring a relatively soft equation of state and excluding seve...
Binary neutron-star mergers: a review of Einstein's richest laboratory
gr-qc 2016-07 accept novelty 2.0 of 10

A comprehensive 2016 survey of binary neutron-star merger simulations, covering numerical methods, initial data, post-merger dynamics, magnetic fields, ejecta and nucleosynthesis, with the field's open questions catalogued.

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5 arXiv papers cite this in 7 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 · 5 sentences without a confident label

Cites it as background 2 papers

Baumgarte and Shapiro [ref] , Tichy [ref] , and East et al [ref] presented formalisms for constructing BNS initial data for spinning neutron stars.

Binary Neutron Stars with Arbitrary Spins in Numerical Relativity · Introduction · 0.80
(ii) In addition to the theme of this review, namely the linking of GW observations to physical properties of the emitting system and in particular the EoS, there is a lot of ongoing work and some robust results also on heavy-element production [ref] and macronovae [ref] , on improved initial data, including better computations of BNS with non-negligibly spinning stars [ref] and BNS with eccentricity [ref] , and on the treatment of physical viscosity [ref] .

Gravitational waves from neutron star mergers and their relation to the nuclear equation of state · Status of numerical-relativity simulations for binary neutron-star mergers · 0.94

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