Angular Momentum Evolution in Dark Matter Halos

(2) Astronomy Department; Alyson Brooks (1); Andrew J. Benson (1); Annika H. G. Peter (1); Fabio Governato (2) ((1) California Institute of Technology; Laura G. Book (1); University of Washington)

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Angular Momentum Evolution in Dark Matter Halos

Laura G. Book (1), Alyson Brooks (1), Annika H. G. Peter (1), Andrew J. Benson (1), Fabio Governato (2) ((1) California Institute of Technology, (2) Astronomy Department, University of Washington)

Astrophysics of Galaxies · Submitted 22 Jun 2010

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

The authors' main claim Since the model of adiabatic contraction that is often applied to model the effects of galaxy evolution on the dark-matter density profile in a halo assumes angular momentum conservation, this variation implies that there is a fundamental limit on the possible accuracy of the adiabatic contraction model in modeling the response of DM halos to the growth of galaxies.

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arXiv ID1006.4365 (version 2)

Pith IDTB6HT34N, Pith's permanent record of this paper and its review

Citation(2) Astronomy Department, Alyson Brooks (1), Andrew J. Benson (1), Annika H. G. Peter (1), Fabio Governato (2) ((1) California Institute of Technology, Laura G. Book (1), University of Washington). "Angular Momentum Evolution in Dark Matter Halos." arXiv:1006.4365 (2010). https://pith.science/paper/TB6HT34N

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,637 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.19 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.83 · compares with prior results 0.31 · mentions code or data availability 0.02.

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

We have analyzed high resolution N-body simulations of dark matter halos, focusing specifically on the evolution of angular momentum. We find that not only is individual particle angular momentum not conserved, but the angular momentum of radial shells also varies over the age of the Universe by up to factors of a few. We find that torques from external structure are the most likely cause for this distribution shift. Since the model of adiabatic contraction that is often applied to model the effects of galaxy evolution on the dark-matter density profile in a halo assumes angular momentum conservation, this variation implies that there is a fundamental limit on the possible accuracy of the adiabatic contraction model in modeling the response of DM halos to the growth of galaxies.

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 have analyzed high resolution N-body simulations of dark matter halos, focusing specifically on the evolution of angular momentum.	contribution 0.53	0.96	0.03	asserted 0.92
s1	We find that not only is individual particle angular momentum not conserved, but the angular momentum of radial shells also varies over the age of the Universe by up to factors of a few.	result 1.00	0.96	0.39	asserted 1.00
s2	We find that torques from external structure are the most likely cause for this distribution shift.	interpretation 0.92	0.81	0.26	hedged possibility 0.94
s3	Since the model of adiabatic contraction that is often applied to model the effects of galaxy evolution on the dark-matter density profile in a halo assumes angular momentum conservation, this variation implies that there is a fundamental limit on the possible accuracy of the adiabatic contraction model in modeling the response of DM halos to the growth of galaxies.	interpretation 1.00	0.44	0.64	asserted 0.75

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

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arXiv listing abstract v2

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full text
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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 have analyzed high resolution N-body simulations of dark matter halos, focusing specifically on the evolution of angular momentum. We find that not only is individual particle angular momentum not conserved, but the angular momentum of radial shells also varies over the age of the Universe by up to factors of a few. We find that torques from external structure are the most likely cause for this distribution shift. Since the model of adiabatic contraction that is often applied to model the effects of galaxy evolution on the dark-matter density profile in a halo assumes angular momentum conservation, this variation implies that there is a fundamental limit on the possible accuracy of the adiabatic contraction model in modeling the response of DM halos to the growth of galaxies.

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1 arXiv paper cite this in 1 sentence

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

What it cites · 3 sentences without a confident label

Cites as background 4 papers

Although these simple models have a mixed track record of matching observations and hydrodynamic simulations of galaxy evolution, they are currently the only predictive models for the effects of galaxy evolution on the dark-matter profile in halos [ref] .

Galaxy-Induced Transformation of Dark Matter Halos · Introduction · 0.83
Although these simple models have a mixed track record of matching observations and hydrodynamic simulations of galaxy evolution, they are currently the only predictive models for the effects of galaxy evolution on the dark-matter profile in halos [ref] .

Testing adiabatic contraction with SDSS elliptical galaxies · Introduction · 0.83
Although these simple models have a mixed track record of matching observations and hydrodynamic simulations of galaxy evolution, they are currently the only predictive models for the effects of galaxy evolution on the dark-matter profile in halos [ref] .

Dark matter response to galaxy formation · Introduction · 0.83

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