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arxiv: 2606.27480 · v1 · pith:2SM3A5X3new · submitted 2026-06-25 · 🌌 astro-ph.GA

Self-interacting dark matter promotes bar formation in disk galaxies

Shashank Dattathri , Frank C. van den Bosch , HanYuan Zhang , Martin D. Weinberg , Eugene Vasiliev , Priyamvada Natarajan , Vasily Belokurov This is my paper

Pith reviewed 2026-06-29 01:26 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords self-interacting dark matterstellar barsdisk galaxiesN-body simulationsangular momentum transferdark matter halosgravothermal collapseresonances
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The pith

Self-interacting dark matter causes bars to form earlier and grow larger in disk galaxies than collisionless dark matter.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper establishes that self-interacting dark matter produces stellar bars that form earlier and reach higher amplitudes than in standard cold dark matter, even with modest interaction strengths. Self-scattering broadens the resonances between the bar and the halo, which increases the rate of angular momentum transfer out of the stellar disk. Disks that stay stable and bar-free under collisionless conditions develop strong bars once self-interactions are included. The acceleration is shown to operate independently of the density cores that SIDM usually creates. At late times, gravothermal core collapse can reverse the effect and weaken or dissolve the bars.

Core claim

Compared with collisionless CDM, SIDM produces bars that form earlier and grow to larger amplitudes, even for modest self-interaction cross sections, because self-interactions broaden the bar-halo resonances and enhance angular momentum transfer from the stellar disk to the halo. Disks that remain stable in CDM, including kinematically hot and dark-matter-dominated disks, develop strong bars in SIDM. This phenomenon is not related to core formation in SIDM halos. At late times, gravothermal core collapse can raise the central dark matter density enough to weaken or dissolve the bar.

What carries the argument

Broadening of bar-halo resonances by dark matter self-interactions, which increases angular momentum transfer from the stellar disk to the halo.

If this is right

  • Bars form earlier and reach higher amplitudes in SIDM than in CDM.
  • Kinematically hot and dark-matter-dominated disks that stay stable in CDM form strong bars once self-interactions are present.
  • The bar acceleration occurs independently of core formation in the halo.
  • Late-time gravothermal collapse can weaken or dissolve bars by raising central density.
  • The abundance, strength, and redshift evolution of bars can constrain the dark matter self-interaction cross section.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Surveys of bar fractions across redshift could provide an independent test of SIDM parameter space.
  • Adding gas and star formation to the simulations would test whether the resonance-broadening effect survives realistic baryonic physics.
  • The same resonance-broadening mechanism might alter the evolution of other non-axisymmetric structures such as spirals or lopsidedness.
  • Morphological statistics from large galaxy samples offer a complementary route to direct detection or other small-scale probes of dark matter interactions.

Load-bearing premise

The idealized N-body setup assumes a collisionless stellar disk with no gas or star formation, and that kinetic theory correctly describes the resonance-broadening process.

What would settle it

High-resolution simulations that find no difference in bar formation time or final amplitude between SIDM and CDM halos, or observations showing that the fraction of barred galaxies at high redshift matches CDM predictions without any acceleration.

Figures

Figures reproduced from arXiv: 2606.27480 by Eugene Vasiliev, Frank C. van den Bosch, Hanyuan Zhang, Martin D. Weinberg, Priyamvada Natarajan, Shashank Dattathri, Vasily Belokurov.

Figure 1
Figure 1. Figure 1: Left: evolution of the central dark matter density (𝜌𝑐) over time for the Fiducial suite of simulations, normalized by its initial value (𝜌𝑐,0). The central density remains constant in the CDM run, while in the SIDM runs, the central density initially drops (core formation) and then rises over time (core collapse). Right: bar amplitude (𝐴2/𝐴0) vs time for the same set of runs. In CDM, the disk is stable ag… view at source ↗
Figure 2
Figure 2. Figure 2: Projected stellar surface density in the x-y plane for the Fiducial suite. The columns correspond to the CDM (left), 𝜎m = 1 cm2 /g (middle), and 𝜎m = 10 cm2 /g (right) runs, with different rows corresponding to different snapshot times, as indicate in the top-left corner of each panel. The bar amplitude is also indicated, in the top-right corner. Note that the CDM run forms a moderate bar only at late time… view at source ↗
Figure 3
Figure 3. Figure 3: Bar amplitude evolution in the various models. Within each panel, the CDM, 𝜎m = 1 cm2 /g, and 𝜎m = 10 cm2 /g runs are plotted. In all cases, the bar amplitude rises faster and reacher a higher value in the SIDM runs compared to CDM. Noteworthy cases are Models A and E, which are stable against bar formation in CDM, but do form bars once the cross section is dialed up. 0 2 4 6 8 10 12 T (Gyr) 10 0 10 1 c c,… view at source ↗
Figure 4
Figure 4. Figure 4: Normalized central dark matter density evolution (left) and bar amplitude vs time for Core suite. As in the Fiducial suite, the central density remains constant throughout in the CDM runs. In the SIDM runs, since the halo begins with an isothermal core, the heat conduction is always outward, resulting in a central dark matter density that continuously increases over time. Despite this, the bar amplitude tr… view at source ↗
Figure 5
Figure 5. Figure 5: Normalized central dark matter density evolution (left) and bar amplitude vs time for the Fiducial CDM (blue) and 𝜎m = 10 cm2 /g (green) runs, and the Freeze 𝑇off = 0.4 Gyr (orange) and 𝑇off = 0.8 Gyr (red) runs. The Freeze simulations are run by freezing the 𝜎m = 10 cm2 /g simulation and turning off the dark matter self-interactions at time 𝑇off, indicated by the dashed vertical lines. After this, the sim… view at source ↗
Figure 6
Figure 6. Figure 6: Change in the total z-component angular momentum Δ𝐿𝑧 of the disk (solid lines) and halo (dashed lines) in the Fiducial suite, normalized by the disk’s initial value 𝐿𝑧,0. In all runs, the disk transfers angular momentum to the halo, and this transfer is more efficient in SIDM, and with increasing cross section, than in CDM. 4.3 Angular momentum transfer between the disk and halo First, we compare the overa… view at source ↗
Figure 7
Figure 7. Figure 7: Change in the halo’s 𝑧-component of angular momentum, ⟨Δ𝐿𝑧 ⟩, between 𝑇 = 10 Gyr and 12 Gyr, binned in the 𝐸 and 𝜅 ≡ 𝐿/𝐿c (𝐸) plane. Both 𝐸 and ⟨Δ𝐿𝑧 ⟩ are in units of 𝐸0 = 1 kpc2 Gyr−2 and 𝐿0 = 1 kpc km s−1 . The left and right panels correspond to the CDM run and to the SIDM run with 𝜎m = 1 cm2 /g, respectively. The black lines represent resonance loci, corresponding to the ultraharmonic resonance (dotted… view at source ↗
Figure 8
Figure 8. Figure 8: Enclosed dark matter fraction within 1 kpc over time in the Fiducial suite. In the CDM run, 𝑓DM(1 kpc) remains constant over time, whereas in the SIDM 𝜎m = 0.1 cm2 /g and 𝜎m = 1 cm2 /g runs it de￾creases out to 5 Gyr due to dark matter core formation. However in the 𝜎m = 10 cm2 /g run, the halo quickly enters core collapse, and the value of 𝑓DM(1 kpc) increases over time after the first ∼ 0.5 Gyr. By the e… view at source ↗
read the original abstract

Despite its remarkable success on large scales, the standard $\Lambda$CDM paradigm faces persistent small-scale challenges that have motivated alternative models for the dark sector. Self-interacting dark matter (SIDM) offers a compelling possibility, in which dark matter particles can scatter off each other. Stellar bars are a ubiquitous feature of disk galaxies across cosmic time. Bars are dynamically coupled to their host galaxy's dark matter halo, and therefore their properties provide a powerful probe of the nature and distribution of dark matter. In this paper, we use idealized, high-resolution $N$-body simulations and analytic calculations based on kinetic theory to study bar formation and evolution in disk galaxies embedded in SIDM halos. We find that compared with collisionless CDM, SIDM produces bars that form earlier and grow to larger amplitudes, even for modest self-interaction cross sections. In several cases, disks that remain stable in CDM, including kinematically hot and dark-matter-dominated disks, develop strong bars in SIDM. This accelerated bar growth occurs because self-interactions broaden the bar-halo resonances and enhance angular momentum transfer from the stellar disk to the halo. We explicitly show that this phenomenon is not related to core formation in SIDM halos. At late times, gravothermal core collapse can raise the central dark matter density enough to weaken or dissolve the bar. These results suggest that the abundance, strength, and redshift evolution of barred galaxies offer a promising observational route to constraining dark matter self-interactions, particularly in light of the growing sample of high-redshift bars revealed by JWST.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript uses idealized high-resolution N-body simulations of stellar disks embedded in SIDM halos together with analytic kinetic-theory calculations to argue that, relative to collisionless CDM, even modest self-interaction cross sections cause bars to form earlier and reach larger amplitudes. The mechanism is identified as self-interaction-induced broadening of bar-halo resonances that enhances angular-momentum transfer from the disk to the halo; the effect is stated to be independent of core formation. Late-time gravothermal collapse is shown to raise central density and can weaken or dissolve bars. The results are presented as a potential observational constraint on SIDM via the statistics and redshift evolution of barred galaxies.

Significance. If the resonance-broadening channel is confirmed to dominate, the work supplies a concrete, falsifiable link between a microscopic dark-matter property and a macroscopic galactic morphology observable, complementing existing SIDM tests and timely with JWST high-redshift bar detections. The dual use of forward N-body integrations and analytic kinetic theory is a methodological strength.

major comments (3)
  1. [§4] §4 (kinetic-theory section): the mapping from the analytic scattering operator to the simulated torque integrals and resonance widths is asserted but not demonstrated by direct extraction of resonance widths or angular-momentum flux spectra from the particle data; without this quantitative comparison the attribution of the bar-growth difference to resonance broadening remains an assumption rather than a verified result.
  2. [§3] §3 (simulation setup): the idealized collisionless stellar disk (no gas, no star formation) leaves the central claim vulnerable to the possibility that baryonic processes alter disk velocity dispersion or halo response enough to erase or reverse the reported SIDM acceleration; a controlled comparison run including gas would be required to establish robustness.
  3. [Results] Results (e.g., Figures 3–5 and associated text): the statement that the bar-growth difference is independent of core formation needs an explicit control showing that the same cross-section values produce the reported effect even when core size is held fixed or minimized; the current separation of the two phenomena is stated but not quantitatively isolated.
minor comments (2)
  1. [Abstract] Abstract: the phrase 'in several cases' for disks that remain stable in CDM should be replaced by an explicit count or fraction of the simulated suite.
  2. [Figures] Figure captions: cross-section values (in cm² g⁻¹) should be stated explicitly in every panel or caption rather than referenced only in the text.

Simulated Author's Rebuttal

3 responses · 1 unresolved

We thank the referee for their constructive and detailed comments. We address each major point below and indicate where revisions will be made to strengthen the manuscript.

read point-by-point responses

  1. Referee: [§4] §4 (kinetic-theory section): the mapping from the analytic scattering operator to the simulated torque integrals and resonance widths is asserted but not demonstrated by direct extraction of resonance widths or angular-momentum flux spectra from the particle data; without this quantitative comparison the attribution of the bar-growth difference to resonance broadening remains an assumption rather than a verified result.

    Authors: We agree that a direct quantitative link would strengthen the attribution. In the revised manuscript we will extract resonance widths and angular-momentum flux spectra directly from the simulation particle data and compare them to the analytic predictions, adding this comparison as a new figure and subsection in §4. revision: yes

  2. Referee: [§3] §3 (simulation setup): the idealized collisionless stellar disk (no gas, no star formation) leaves the central claim vulnerable to the possibility that baryonic processes alter disk velocity dispersion or halo response enough to erase or reverse the reported SIDM acceleration; a controlled comparison run including gas would be required to establish robustness.

    Authors: Our study deliberately employs an idealized collisionless setup to isolate the SIDM-driven dynamical mechanism. While baryonic processes could modulate the outcome, the resonance-broadening channel is a dark-matter effect whose qualitative impact should persist. We will add an expanded discussion of this limitation and possible baryonic influences in the revised text. revision: partial

  3. Referee: [Results] Results (e.g., Figures 3–5 and associated text): the statement that the bar-growth difference is independent of core formation needs an explicit control showing that the same cross-section values produce the reported effect even when core size is held fixed or minimized; the current separation of the two phenomena is stated but not quantitatively isolated.

    Authors: The existing suite already includes runs at early times and modest cross sections where core formation is negligible. To make the separation fully quantitative we will add a dedicated control set with parameters chosen to suppress core growth while retaining self-interactions, demonstrating that the bar-acceleration effect remains. revision: yes

standing simulated objections not resolved
  • Request for new controlled simulations that include gas and star formation, which would require substantial additional model development and computational resources outside the present scope.

Circularity Check

0 steps flagged

No circularity; results from direct N-body integrations and independent kinetic theory

full rationale

The paper derives its claims from forward N-body simulations initialized with standard disk+halo conditions and from separate analytic kinetic-theory estimates of resonance broadening; neither step fits parameters to the bar-formation outcomes and then re-labels them as predictions, nor does any load-bearing step reduce to a self-citation or self-defined quantity. The headline attribution of accelerated bar growth to resonance broadening is therefore an output of the integrations rather than an input by construction.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the validity of Newtonian N-body dynamics for the stellar component, the kinetic-theory treatment of dark-matter self-scattering, and the choice of modest velocity-independent cross sections; no new particles or forces are introduced.

free parameters (1)
  • self-interaction cross section per unit mass
    Modest values are selected for the runs; the precise numerical values function as free parameters that control the strength of the reported effect.
axioms (2)
  • standard math Newtonian gravity and collisionless stellar dynamics govern the disk and halo particles
    Invoked throughout the N-body component of the study.
  • domain assumption Kinetic theory provides an accurate description of the broadened bar-halo resonances under self-interactions
    Used to derive the analytic explanation for the accelerated angular-momentum transfer.

pith-pipeline@v0.9.1-grok · 5847 in / 1384 out tokens · 43974 ms · 2026-06-29T01:26:53.361341+00:00 · methodology

discussion (0)

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Reference graph

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