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arxiv: 2606.08628 · v1 · pith:CYJTXCT6new · submitted 2026-06-07 · 🌌 astro-ph.HE · astro-ph.CO

Thermal emission from dark matter-heated neutron stars in the Galactic Center

Yunhe Hu , Feng Huang , Taotao Fang This is my paper

Pith reviewed 2026-06-27 17:51 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.CO
keywords dark matterneutron starsGalactic Centerthermal emissiondark matter annihilationinterstellar extinctionsurface temperature
0
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The pith

Dark matter heating leaves neutron stars in the Galactic Center below current detection limits

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

The paper calculates how dark matter particles captured by neutron stars in the Galactic Center annihilate and deposit heat inside the stars. For neutron stars older than roughly 10 million years this heating reaches balance with the stars' natural cooling, producing equilibrium surface temperatures from 10,000 to 1 million Kelvin depending on the local dark matter density. Even when a central density spike raises the temperature and shifts the emission toward ultraviolet and soft X-rays, heavy interstellar extinction and high column densities suppress the light from any single star to below 0.1 nanoJansky. The summed infrared glow from the entire population of such stars stays under 10^{-9} Jy per square arcsecond. These numbers place the predicted signals below the reach of present instruments, though the authors note that lower-extinction sight lines could improve the prospects.

Core claim

Neutron stars older than about 10 million years in the Galactic Center reach an equilibrium surface temperature of 10^4 to 10^6 K set by the balance between heating from dark matter capture and annihilation and the star's cooling. The temperature depends on location and the ambient dark matter density profile, which the authors vary from cored to cuspy forms that may include a central spike. With a spike the emission would appear in ultraviolet and soft X-ray bands, yet strong interstellar extinction and large hydrogen column densities reduce the observable flux density from an individual star to below 0.1 nJy. The integrated emission from the whole neutron star population produces an averag

What carries the argument

Equilibrium surface temperature reached when dark matter capture and annihilation heating balances neutron star cooling, evaluated across cored-to-cuspy dark matter density profiles that may include spikes.

If this is right

  • Neutron stars older than 10 million years settle at equilibrium temperatures between 10,000 and 1 million Kelvin.
  • A central dark matter density spike shifts the thermal emission into ultraviolet and soft X-ray bands.
  • Interstellar extinction keeps the flux from any single neutron star below 0.1 nJy.
  • The neutron star population produces a cumulative infrared surface brightness of at most 10^{-9} Jy arcsec^{-2}.
  • Thermal signatures from these stars remain below the sensitivity of current instruments.

Where Pith is reading between the lines

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

  • Similar heating calculations could be applied to neutron stars in other high-density dark matter regions with lower extinction to test the same mechanism.
  • If the equilibrium temperatures are reached, non-detection in deeper surveys would constrain either the dark matter density or the capture efficiency.
  • Future ultraviolet or soft X-ray instruments with greater sensitivity might reach the predicted fluxes if extinction models are refined.
  • The approach could be tested by comparing predicted and observed temperatures for any old neutron stars identified in less obscured fields.

Load-bearing premise

Neutron stars older than about 10 million years reach an equilibrium surface temperature set solely by the balance of dark matter heating against cooling, and the chosen dark matter density profiles correctly describe the ambient density at neutron star locations in the Galactic Center.

What would settle it

A measured surface temperature for an old neutron star in the Galactic Center lying well outside the 10,000 to 1 million Kelvin range, or a detected flux density from an individual star exceeding 0.1 nJy after extinction correction.

Figures

Figures reproduced from arXiv: 2606.08628 by Feng Huang, Taotao Fang, Yunhe Hu.

Figure 1
Figure 1. Figure 1: FIG. 1. DM density profiles are shown as functions of the [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Cooling curves show the time evolution of the core temperature [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Equilibrium thermal properties of NSs located at different galactic radii, as supported by DM heating. The top panels [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Luminosity [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Average surface brightness [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
read the original abstract

We investigate the thermal impact of dark matter (DM) capture and annihilation on neutron stars (NSs) in the Galactic Center (GC). Accounting for both kinetic energy deposition and internal annihilation, we systematically evaluate the influence of various DM density profiles, ranging from cored to cuspy distributions, on the late-time thermal evolution of NSs. For NSs older than $\sim 10^7~\mathrm{yr}$, the surface temperature approaches an equilibrium value $T_\mathrm{s}^{\mathrm{eq}} \sim 10^4$--$10^6~\mathrm{K}$, depending on the stellar location and the ambient DM density. In the presence of a density spike, enhanced heating shifts the emission toward ultraviolet (UV) and soft x-ray bands; however, strong interstellar extinction and large hydrogen column densities significantly suppress the observable flux density. We further provide an estimate of the cumulative infrared surface brightness from the NS population in the GC. The predicted flux density from an individual NS remains below $\sim 0.1\,\mathrm{nJy}$, while the integrated emission yields an average surface brightness $I_\nu \lesssim 10^{-9}\,\mathrm{Jy\,arcsec^{-2}}$, corresponding to a signal-to-noise ratio well below current detection thresholds. Our results indicate that thermal signatures from DM-heated NSs in the GC remain below the sensitivity limits of current instruments, although nearby systems with lower extinction may provide more promising targets for detection.

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

1 major / 2 minor

Summary. The paper examines the thermal effects of dark matter capture and annihilation heating on neutron stars in the Galactic Center. It evaluates multiple DM density profiles (cored to cuspy with spikes) and finds that NSs older than ~10^7 yr reach equilibrium surface temperatures of 10^4--10^6 K. Enhanced heating from density spikes shifts emission to UV/soft X-rays, but interstellar extinction suppresses the observable flux; individual NS fluxes are predicted below ~0.1 nJy and the integrated surface brightness below 10^{-9} Jy arcsec^{-2}, remaining below current instrument thresholds. Nearby systems with lower extinction are suggested as better targets.

Significance. If the equilibrium temperature calculations and extinction modeling hold, the result indicates that DM-heated NS thermal signatures in the GC are not detectable with present instruments, while identifying lower-extinction nearby targets as more promising. The systematic comparison across DM profiles is a strength, as is the explicit inclusion of both kinetic deposition and annihilation heating.

major comments (1)
  1. [§4 (equilibrium temperature and flux estimates)] The central claim that fluxes remain below detection thresholds rests on the equilibrium temperature reached for NSs ≳10^7 yr. The manuscript should provide an explicit sensitivity test (e.g., in §4 or §5) showing how the adopted DM density profiles and spike parameters propagate into the final flux upper limits; without this, the conclusion that signals are undetectable is tied to the weakest modeling assumption.
minor comments (2)
  1. [Abstract] The abstract states T_s^eq ~10^4--10^6 K but does not reference the specific cooling curves or capture-rate formulae used; adding a brief pointer to the relevant equations would improve traceability.
  2. [Results section on integrated emission] Figure captions (or the text near the cumulative brightness estimate) should clarify whether the reported I_ν includes only the DM-heated component or also standard NS cooling.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive feedback and positive assessment of the manuscript. We address the single major comment below.

read point-by-point responses

  1. Referee: [§4 (equilibrium temperature and flux estimates)] The central claim that fluxes remain below detection thresholds rests on the equilibrium temperature reached for NSs ≳10^7 yr. The manuscript should provide an explicit sensitivity test (e.g., in §4 or §5) showing how the adopted DM density profiles and spike parameters propagate into the final flux upper limits; without this, the conclusion that signals are undetectable is tied to the weakest modeling assumption.

    Authors: We agree that an explicit sensitivity test would improve clarity. While the manuscript already systematically varies DM density profiles (cored to cuspy with spikes) and reports the resulting equilibrium temperature range of 10^4--10^6 K, we will add a dedicated paragraph and table in the revised §4 (or new §5 subsection) that explicitly maps each profile and spike parameter set to the corresponding equilibrium temperature, emitted spectrum, and attenuated flux upper limit. This will demonstrate that even the highest-heating (spiked) cases yield individual fluxes ≲0.1 nJy and integrated surface brightness ≲10^{-9} Jy arcsec^{-2} after extinction, confirming the non-detection conclusion is robust across the modeled range. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper computes NS equilibrium temperatures from the balance of DM capture/annihilation heating against cooling, then derives fluxes using external DM density profiles (cored to cuspy with spikes) and standard capture rates. No steps in the abstract or described chain reduce by construction to fitted inputs, self-definitions, or load-bearing self-citations; the below-threshold result follows from these independent inputs without renaming or tautological reduction. This is consistent with the reader's score of 2.0 and the absence of any quoted internal inconsistency.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Only the abstract is available, so the ledger is necessarily incomplete; the central claim rests on standard domain assumptions about DM-NS interactions and equilibrium cooling that are not derived in the provided text.

axioms (2)
  • domain assumption DM capture and annihilation deposit energy that can balance NS cooling for old stars
    Invoked to reach the equilibrium temperature claim for NS older than 10^7 yr.
  • domain assumption DM density profiles (cored to cuspy with spikes) correctly describe the ambient density at NS locations
    Used to vary the heating rate and resulting temperatures.

pith-pipeline@v0.9.1-grok · 5793 in / 1532 out tokens · 25844 ms · 2026-06-27T17:51:39.155357+00:00 · methodology

discussion (0)

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