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The Effect of Gas Cooling on the Shapes of Dark Matter Halos
Astrophysics · Submitted 10 May 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that halos formed in simulations with gas cooling are significantly more spherical than corresponding halos formed in adiabatic simulations.
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The abstract, sentence by sentence
We analyze the effect of dissipation on the shapes of dark matter (DM) halos using high-resolution cosmological gasdynamics simulations of clusters and galaxies in the LCDM cosmology. We find that halos formed in simulations with gas cooling are significantly more spherical than corresponding halos formed in adiabatic simulations. Gas cooling results in an average increase of the principle axis ratios of halos by ~ 0.2-0.4 in the inner regions. The systematic difference decreases slowly with radius but persists almost to the virial radius. We argue that the differences in simulations with and without cooling arise both during periods of quiescent evolution, when gas cools and condenses toward the center, and during major mergers. We perform a series of high-resolution N-body simulations to study the shapes of remnants in major mergers of DM halos and halos with embedded stellar disks. In the DM halo-only mergers, the shape of the remnants depends only on the orbital angular momentum of the encounter and not on the internal structure of the halos. However, significant shape changes in the DM distribution may result if stellar disks are included. In this case the shape of the DM halos is correlated with the morphology of the stellar remnants.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We analyze the effect of dissipation on the shapes of dark matter (DM) halos using high-resolution cosmological gasdynamics simulations of clusters and galaxies in the LCDM cosmology. | contribution 0.76 | 0.94 | 0.04 | asserted 0.71 |
| s1 | We find that halos formed in simulations with gas cooling are significantly more spherical than corresponding halos formed in adiabatic simulations. | result 1.00 | 0.97 | 0.83 | asserted 1.00 |
| s2 | Gas cooling results in an average increase of the principle axis ratios of halos by ~ 0.2-0.4 in the inner regions. | result 1.00 | 0.95 | 0.23 | asserted 1.00 |
| s3 | The systematic difference decreases slowly with radius but persists almost to the virial radius. | result 1.00 | 0.92 | 0.10 | asserted 1.00 |
| s4 | We argue that the differences in simulations with and without cooling arise both during periods of quiescent evolution, when gas cools and condenses toward the center, and during major mergers. | interpretation 1.00 | 0.65 | 0.15 | asserted 0.57 |
| s5 | We perform a series of high-resolution N-body simulations to study the shapes of remnants in major mergers of DM halos and halos with embedded stellar disks. | method 0.74 | 0.95 | 0.02 | asserted 0.83 |
| s6 | In the DM halo-only mergers, the shape of the remnants depends only on the orbital angular momentum of the encounter and not on the internal structure of the halos. | result 1.00 | 0.91 | 0.05 | asserted 1.00 |
| s7 | However, significant shape changes in the DM distribution may result if stellar disks are included. | result 0.99 | 0.83 | 0.07 | hedged possibility 1.00 |
| s8 | In this case the shape of the DM halos is correlated with the morphology of the stellar remnants. | result 0.99 | 0.88 | 0.08 | asserted 1.00 |
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Original abstract
We analyze the effect of dissipation on the shapes of dark matter (DM) halos using high-resolution cosmological gasdynamics simulations of clusters and galaxies in the LCDM cosmology. We find that halos formed in simulations with gas cooling are significantly more spherical than corresponding halos formed in adiabatic simulations. Gas cooling results in an average increase of the principle axis ratios of halos by ~ 0.2-0.4 in the inner regions. The systematic difference decreases slowly with radius but persists almost to the virial radius. We argue that the differences in simulations with and without cooling arise both during periods of quiescent evolution, when gas cools and condenses toward the center, and during major mergers. We perform a series of high-resolution N-body simulations to study the shapes of remnants in major mergers of DM halos and halos with embedded stellar disks. In the DM halo-only mergers, the shape of the remnants depends only on the orbital angular momentum of the encounter and not on the internal structure of the halos. However, significant shape changes in the DM distribution may result if stellar disks are included. In this case the shape of the DM halos is correlated with the morphology of the stellar remnants.
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How the literature uses it
11 arXiv papers cite this in 12 sentences
Papers whose main result relates to this one's
States the same result 1 paper
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First, we show that halos formed in simulations with gas cooling are significantly rounder than halos formed in dissipationless $N$-body simulations.
Dark Matter Halos: Shapes, The Substructure Crisis, and Indirect Detection · 0.98
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