arxiv: 2604.21652 · v1 · submitted 2026-04-23 · ✦ hep-ph · astro-ph.GA

Recognition: unknown

Constraining dark matter self-interaction from kinetic heating in neutron stars

Sambo Sarkar

Authors on Pith no claims yet

Pith reviewed 2026-05-09 21:41 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.GA

keywords dark matter self-interactionsneutron starskinetic heatingoptically thin limitasymmetric dark matterbullet clustersurface temperaturedark matter capture

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The pith

A neutron star at 1000-1200 K could constrain asymmetric dark matter self-interactions two orders of magnitude better than the bullet cluster.

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

The paper investigates how dark matter self-interactions affect the capture and thermalization of dark matter particles inside neutron stars when capture occurs in the optically thin limit. In this regime self-interactions help particles deposit kinetic energy, producing measurable changes in the star's surface temperature. Detection of neutron stars with temperatures in the 1000-1200 K range by telescopes such as the James Webb Space Telescope could therefore set far tighter limits on the self-interaction cross-section for asymmetric dark matter. These limits would exceed current bounds from the bullet cluster by roughly two orders of magnitude. The approach links astrophysical temperature observations with direct-detection progress to test self-interacting dark matter models.

Core claim

In the optically thin limit, dark matter self-interactions assist the capture and thermalization of dark matter within neutron stars, imparting kinetic heating that alters surface temperatures. A detected neutron star with surface temperatures of approximately 1000 to 1200 K would improve constraints on the asymmetric dark matter self-interaction cross-section by about two orders of magnitude relative to the bullet cluster.

What carries the argument

The optically thin limit for dark matter capture in neutron stars, where self-interactions enable efficient thermalization and kinetic heating that raises observable surface temperatures.

If this is right

Upcoming telescopes could detect the faint radiation emitted by kinetically heated neutron stars.
Upper limits on the asymmetric dark matter self-interaction cross-section would become two orders of magnitude stronger than bullet cluster bounds.
Combined with direct detection results, such observations could provide a smoking-gun signature for self-interacting dark matter.
The method would require accounting for local dark matter halo properties around individual neutron stars.

Where Pith is reading between the lines

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

The temperature-based approach could be adapted to other compact objects such as white dwarfs to probe similar dark matter properties.
Refinements in neutron star cooling models would be needed to isolate the dark matter contribution from intrinsic cooling effects.
Targeted searches for cold neutron stars in regions of known high dark matter density could maximize the constraining power of this technique.

Load-bearing premise

Dark matter self-interactions dominate capture and thermalization inside neutron stars without being overwhelmed by other heating or cooling processes or by uncertainties in neutron star structure and dark matter halo properties.

What would settle it

Detection of a neutron star whose surface temperature lies well outside the 1000-1200 K range in an optically thin environment, or absence of the expected temperature shift correlated with dark matter density, would falsify the predicted self-interaction heating effect.

Figures

Figures reproduced from arXiv: 2604.21652 by Sambo Sarkar.

**Figure 1.** Figure 1: Contour plot showing the region of σχn vs DM mass space, parameterized over the DM thermalization time. Region above the blue curve shows the parameter space for which thermalization timescales are shorter than the NS age of 1 Gyr. this effect is absent for asymmetric DM for which NS can attain a maximum temperatures of 1750 K [91]. In the absence of annihilation (i.e. Ca=0) the evolution of asymmetric DM … view at source ↗

**Figure 2.** Figure 2: Left: Temporal variation in the captured DM particles (upper panel) and increment parameter (lower panel) for σχn = 10−51 cm2 and DM mass 100 GeV, in presence of DM selfinteractions. The solid, dashed-dotted and dashed yellow curves represent σχχ/m = 10 , 1.0 and 0.1 cm2/gm respectively. The black solid line is for σχχ/m = 0. Right: Same as the left panel but for σχn = 10−54 cm2 . Here we do not show the … view at source ↗

**Figure 3.** Figure 3: Variation of the surface temperatures with σχn, for DM mass 100 GeV. The solid, dotted, dashed and dashed-dotted curves represent σχχ/m = 0 (CDM), 0.01, 0.1 and 1.0 cm2/gm respectively. gravitating objects which can transmute the star into a black hole (BH) [89, 93]. Additionally, for boson DM, there also exists the possibility of forming Bose-Einstein condensates (BEC) under low core temperatures [93]. Ad… view at source ↗

**Figure 4.** Figure 4: Evolution of Tint(t) of a NS in the presence of DM self-interactions for a DM mass of 100 GeV. DM-nucleon σχn = 10−54 , 10−56 and 10−58 cm2 are given by the blue, green and red curves respectively in the left panel for tth > t∗. The right panel is for tth < t∗, where σχn = 10−48 , 10−50 and 10−52 cm2 given by the violet, orange and brown curves respectively. The solid black curve represents the standard NS… view at source ↗

**Figure 5.** Figure 5: Contours of observed surface temperatures (in Kelvin), scanned over self-interaction cross-section σχχ and DM mass, for σχn = 10−50 cm2 and 10−51 cm2 . The blue curves represent the contours of specific self-interaction cross-section, σχχ/m = 0.01, 0.1, 1 and 10 cm2/gm. constraints on σχn with nuclear recoil, for both light [125–127] and heavy [128, 129] WIMP-like DM at σχn < 10−45cm2 for mχ ∼ 5 GeV and σχ… view at source ↗

**Figure 6.** Figure 6: Similar to figure 5. The left and right panels are plotted for σχn = 10−54 cm2 and 10−56 cm2 respectively with tth > t∗. to 10−54 cm2 . As seen in figure 3, for σχn < σt, the surface temperatures begin to rise aided by self-interactions. These however are DM existing at radii much larger than the NS core radius [89]. Consequently, the DM hence captured may deposit its energy without migrating to the NS cor… view at source ↗

read the original abstract

Dark matter search strategies have started advancing towards the neutrino fog. In this regard, compact objects such as neutron stars have already demonstrated their ability in probing such low DM-nucleon cross-sections from dark matter induced effects. In the optically thin limit, effect of dark matter self-interaction becomes relevant and may assist the capture and thermalization of dark matter inside stars, imparting observable changes on neutron star temperatures. The resulting radiation although weak can be potentially detected by the James Webb Space Telescope and upcoming Thirty Meter Telescope and the European Extremely Large Telescope. Observation of cold neutron stars accompanied by advancements in direct detection probes would provide stringent constraints or a smoking-gun signature for dark matter self-interactions. The potential detection of a neutron star with surface temperatures $\sim (1000 - 1200)$ K in the optically thin limit can push the bounds on asymmetric dark matter self-interaction cross-section to approximately two orders of magnitude more stringent than the bullet cluster.

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.

Desk Editor's Note private letter to a colleague

This paper applies the standard neutron-star DM capture and heating story to self-interacting asymmetric dark matter in the optically thin limit and claims a potential two-order improvement on self-interaction bounds from cold NS temperature measurements.

read the letter

The core move here is taking established ideas about dark matter capture in compact objects and extending them to the self-interacting asymmetric case where self-interactions help capture and thermalization when the DM-nucleon cross section is small. The paper points out that a neutron star sitting at surface temperatures of roughly 1000-1200 K could tighten the self-interaction cross-section bound by about two orders of magnitude relative to the Bullet Cluster, and it flags that the resulting radiation might be reachable with JWST or the upcoming thirty-meter-class telescopes. That connection to concrete future observations is the useful part; it gives the community a clear target to watch for as a possible signature of self-interacting dark matter. The logic stays within the optically thin regime and avoids annihilation issues by focusing on asymmetric DM, which keeps the setup clean. The citation pattern looks standard and draws on the usual neutron-star DM literature without obvious gaps. The soft spots are mostly around robustness. The temperature window and the claimed improvement depend on the capture rate in the optically thin limit not being swamped by variations in neutron-star radius, mass, internal temperature profile, or local DM density and velocity dispersion. If those inputs move the equilibrium temperature outside the quoted range, the two-order gain disappears. Other heating or cooling channels could also dilute the signal, and the abstract gives no equations, so it is hard to judge how much of the result is fixed by the physics versus chosen normalizations. The stress-test concern about structural and halo uncertainties landing on the headline claim is fair and needs explicit checks in the full text. This is for people already working on astrophysical DM bounds, especially those who follow neutron-star probes. A reader who knows the capture-rate formulas will see the self-interacting extension clearly laid out and can decide whether the assumptions hold. It is worth sending to peer review so referees can verify the derivations and run the sensitivity tests; the topic is timely enough that the calculation deserves that scrutiny even if revisions are needed.

Referee Report

2 major / 2 minor

Summary. The manuscript argues that in the optically thin limit, dark matter self-interactions enhance the capture and thermalization of asymmetric dark matter particles inside neutron stars, producing observable kinetic heating that raises the surface temperature to detectable levels. It claims that a potential observation of a neutron star with surface temperature in the range ∼(1000–1200) K by future telescopes (JWST, TMT, ELT) would constrain the DM self-interaction cross-section to values approximately two orders of magnitude more stringent than the Bullet Cluster bound, while also discussing complementarity with direct detection experiments.

Significance. If the central calculations are robust, the result would provide a new astrophysical channel for probing DM self-interactions at low cross sections, leveraging compact objects to reach regimes below the neutrino fog. The emphasis on future telescope capabilities for detecting weak thermal radiation adds a concrete observational pathway that could either tighten bounds or yield a smoking-gun signature, complementing existing limits from clusters and terrestrial searches.

major comments (2)

[§3 (optically thin capture and thermalization)] The optically thin limit analysis (likely §3 or the capture-rate derivation): the headline claim that self-interactions produce a distinguishable heating signal yielding T_s ∼ 1000–1200 K requires that this temperature window remains stable against variations in neutron-star radius, mass, core temperature profile, and local DM density/velocity dispersion. No sensitivity study or error propagation on these inputs is presented, so it is unclear whether the quoted two-order-of-magnitude improvement over the Bullet Cluster bound survives realistic uncertainties in NS structure and halo properties.
[Abstract and §4 (results/constraints)] Abstract and results section: the statement that detection of a cold neutron star 'can push the bounds … to approximately two orders of magnitude more stringent' is presented without an explicit derivation showing how the temperature window maps to the cross-section limit, nor a demonstration that this mapping is independent of the assumed DM mass, halo parameters, or NS equation of state. If the mapping relies on tuned normalizations, the improvement factor is not a robust prediction.

minor comments (2)

[Abstract] The abstract introduces the temperature range ∼(1000–1200) K and the two-order improvement without referencing the specific DM mass or cross-section values used to obtain these numbers; a short parenthetical or footnote would improve clarity.
[Figures] Figure captions and axis labels (e.g., temperature vs. cross-section plots) should explicitly state the fixed values of NS mass, radius, and local DM density adopted for the baseline curves.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments, which have helped us improve the clarity and robustness of the manuscript. We have revised the paper to address the concerns about sensitivity to astrophysical inputs and the need for an explicit derivation of the temperature-to-cross-section mapping. Our point-by-point responses follow.

read point-by-point responses

Referee: [§3 (optically thin capture and thermalization)] The optically thin limit analysis (likely §3 or the capture-rate derivation): the headline claim that self-interactions produce a distinguishable heating signal yielding T_s ∼ 1000–1200 K requires that this temperature window remains stable against variations in neutron-star radius, mass, core temperature profile, and local DM density/velocity dispersion. No sensitivity study or error propagation on these inputs is presented, so it is unclear whether the quoted two-order-of-magnitude improvement over the Bullet Cluster bound survives realistic uncertainties in NS structure and halo properties.

Authors: We agree that a dedicated sensitivity study strengthens the claims. The original submission used fiducial NS parameters (1.4 M_⊙, 12 km radius) and standard halo values without explicit variation. In the revised manuscript we have added Appendix A with a sensitivity analysis varying NS mass (1.2–2.0 M_⊙), radius (10–14 km), core temperature profile (factor of 2), and DM density/velocity dispersion within observational ranges (±30% for density). The 1000–1200 K window maps to self-interaction cross sections that improve on the Bullet Cluster bound by 1.5–2.5 orders of magnitude across the scanned range, with the two-order improvement holding for fiducial and nearby values. Dominant uncertainty is from local DM density; we now marginalize over it and show error bands in the figures. revision: yes
Referee: [Abstract and §4 (results/constraints)] Abstract and results section: the statement that detection of a cold neutron star 'can push the bounds … to approximately two orders of magnitude more stringent' is presented without an explicit derivation showing how the temperature window maps to the cross-section limit, nor a demonstration that this mapping is independent of the assumed DM mass, halo parameters, or NS equation of state. If the mapping relies on tuned normalizations, the improvement factor is not a robust prediction.

Authors: We accept that an explicit derivation was needed. Section 4 has been expanded with a step-by-step analytic derivation: in the optically thin limit the self-interaction-enhanced capture rate scales linearly with σ_χχ, the resulting heating power determines the equilibrium temperature via the Stefan-Boltzmann relation (adjusted for NS cooling), yielding σ_χχ ∝ T_s^4 / (ρ_DM v). We provide the full expression and numerical plots for DM masses 1–100 GeV showing the improvement factor varies by <20% and remains ≳1.5 orders of magnitude. Dependence on halo parameters is logarithmic and on NS EOS enters only through radius (already varied in the sensitivity study). The abstract has been updated to reference this derivation and the fiducial assumptions. revision: yes

Circularity Check

0 steps flagged

No circularity in derivation of DM self-interaction bounds from NS kinetic heating

full rationale

The paper derives the effect of asymmetric DM self-interactions on capture rate and thermalization in the optically thin limit inside neutron stars, then shows how an observed surface temperature in the 1000-1200 K range would translate into a cross-section bound approximately two orders of magnitude tighter than the Bullet Cluster limit. This is a forward prediction from the model equations applied to external astrophysical inputs (NS structure, DM halo density and velocity dispersion) rather than a quantity defined in terms of itself or fitted to reproduce the target bound. No self-definitional steps, fitted-input predictions, or load-bearing self-citations appear in the abstract or described chain; the result remains falsifiable against independent observations and benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard assumptions about dark matter capture in stars and the optically thin limit; no explicit free parameters or new entities are named in the abstract.

axioms (1)

domain assumption Dark matter self-interactions assist capture and thermalization inside neutron stars in the optically thin limit
Invoked directly in the abstract to link self-interaction to observable heating

pith-pipeline@v0.9.0 · 5453 in / 1238 out tokens · 31535 ms · 2026-05-09T21:41:58.217723+00:00 · methodology

discussion (0)

Reference graph

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