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arxiv: 2511.07567 · v2 · submitted 2025-11-10 · 🌌 astro-ph.HE

Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach

Adamu Issifu , Prashant Thakur , Davood Rafiei Karkevandi , Franciele M. da Silva , D\'ebora P. Menezes , Y. Lim , Tobias Frederico This is my paper

Pith reviewed 2026-05-17 23:07 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords dark matterproto-neutron starstwo-fluid modelneutron star coolinggravitational interactionhyperonsKelvin-Helmholtz timescalesupernova neutrinos
0
0 comments X

The pith

Dark matter cores in proto-neutron stars heat ordinary matter by deepening the gravitational potential, while extended halos cool it.

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

The paper establishes that non-annihilating asymmetric dark matter, interacting with ordinary matter only through gravity, produces opposite thermal effects in evolving proto-neutron stars depending on its spatial distribution. Dense dark matter cores pull ordinary matter inward, raising its temperature, whereas diffuse dark matter halos supply external support that lowers the temperature. These changes also alter the onset of hyperons and the overall particle profiles in ways that differ from the softening caused by exotic baryons alone. The resulting signatures appear most strongly during deleptonization and the neutrino-transparent phase, offering a potential observational window through supernova neutrino signals and early pulsar cooling.

Core claim

In the two-fluid quasi-static model of protoneutron-star evolution over the Kelvin-Helmholtz timescale, dark matter cores deepen the gravitational potential and thereby compress and heat the baryonic matter, while extended dark matter halos provide external support that leads to cooling; hyperons and other exotic baryons produce a similar softening of the equation of state but reduce rather than increase temperature, so the distinct temperature and composition profiles serve as a diagnostic of dark matter presence.

What carries the argument

Quasi-static two-fluid framework treating dark matter and ordinary matter as separate fluids coupled solely by gravity and evolved across the Kelvin-Helmholtz cooling timescale.

If this is right

  • Dark matter cores increase the compactness of the star and shift the density at which hyperons first appear.
  • The strongest modifications to temperature and composition occur during the deleptonization and neutrino-transparent stages.
  • The altered early thermal history imprints on supernova neutrino light curves and on the cooling tracks of young pulsars.
  • The presence of dark matter can be distinguished from the effects of hyperons because the former raises temperature while the latter lowers it.

Where Pith is reading between the lines

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

  • If the predicted temperature contrast is confirmed, it could be used to place limits on the captured dark matter mass inside neutron stars formed in supernovae.
  • The same gravitational coupling mechanism may affect the stability or merger dynamics of older neutron stars that have accumulated dark matter over time.
  • Future multi-messenger data combining neutrino detections with precise mass-radius measurements of young pulsars could test the two-fluid predictions directly.

Load-bearing premise

Dark matter interacts with ordinary matter only through gravity, remains non-annihilating and asymmetric, and the quasi-static two-fluid treatment fully captures the thermal and compositional changes without instabilities.

What would settle it

Observation of the temperature evolution or neutrino emission from a young neutron star that shows neither the predicted heating for compact dark matter cores nor the predicted cooling for extended halos, when compared against standard models without dark matter.

Figures

Figures reproduced from arXiv: 2511.07567 by Adamu Issifu, Davood Rafiei Karkevandi, D\'ebora P. Menezes, Franciele M. da Silva, Prashant Thakur, Tobias Frederico, Y. Lim.

Figure 1
Figure 1. Figure 1: FIG. 1. Variation of the core pressure of a 1 [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Particle distribution profiles versus normalized radius for a PNS with [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Mass–radius relations for PNS models with and without DM. The first panel shows hot PNSs configurations, including [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Temperature profiles as a function of normalized radius [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Radial temperature profiles for dark matter halo [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Temperature as a function of gravitational mass for different entropy per baryon and lepton fraction conditions. The left [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
read the original abstract

Neutron stars (NSs) provide a unique laboratory to probe dark matter (DM) through its gravitational imprint on stellar evolution. We use a two-fluid framework with non-annihilating, asymmetric DM, both fermionic and bosonic, that interacts with ordinary matter (OM) solely through gravity. Within this framework, we track protoneutron stars (PNSs) across their thermal and compositional evolution via quasi-static modeling over the Kelvin--Helmholtz cooling timescale. We uncover a distinct thermal signature: DM cores deepen the gravitational potential, compressing and heating the baryonic matter, while extended DM halos provide external support, leading to cooling of the stellar matter. In contrast, hyperons and other exotic baryons soften the equation of state similarly to DM cores but reduce, rather than increase, the temperature. DM thus alters both temperature and particle distribution profiles in ways that provide a clear diagnostic of its presence. DM cores also enhance compactness and shift hyperon onset, with the strongest effects during deleptonization and neutrino-transparent phases due to reduced neutrino pressure contributions. Consequently, this early thermal evolution, observable through supernova neutrino light curves and young pulsar cooling curves, offers a direct, testable probe of DM in NSs.

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

2 major / 2 minor

Summary. The manuscript develops a two-fluid hydrostatic model for evolving protoneutron stars that includes a dark matter component interacting only gravitationally. The authors evolve the system quasi-statically over the Kelvin-Helmholtz cooling phase for both fermionic and bosonic DM, reporting that compact DM cores increase the central temperature of the baryonic fluid through gravitational compression while diffuse DM halos decrease it through external pressure support. They contrast this with the effect of hyperons, which soften the equation of state but lower the temperature, and suggest that the resulting temperature and composition profiles could be diagnosed through supernova neutrino signals and early pulsar cooling curves.

Significance. If the central thermal signatures are robust, the work supplies a concrete, observationally accessible diagnostic that distinguishes gravitational DM effects from other exotic degrees of freedom such as hyperons. The emphasis on the deleptonization and neutrino-transparent epochs targets a phase where neutrino pressure is low and structural sensitivity to the DM potential is high, potentially linking to supernova neutrino light curves and young pulsar cooling data.

major comments (2)
  1. [Modeling section / quasi-static evolution] The quasi-static two-fluid hydrostatic solutions are evolved over the full Kelvin-Helmholtz timescale, yet no stability analysis or timescale-separation argument is supplied to demonstrate that convective or dynamical readjustments remain negligible precisely when neutrino pressure support drops (the regime where the largest temperature contrasts are reported). Without such checks the predicted heating/cooling signatures could be artifacts of the approximation rather than genuine gravitational imprints.
  2. [Results on thermal signatures] The manuscript states that DM cores deepen the gravitational potential and thereby heat the baryonic matter while halos provide external support and cool it, but no quantitative comparison is given to the temperature profiles obtained in the corresponding single-fluid PNS models or to standard limits (e.g., zero-DM case). This makes it difficult to judge the magnitude and robustness of the claimed thermal diagnostic.
minor comments (2)
  1. [Introduction / Methods] Notation for the two-fluid gravitational potential and the separate density profiles should be introduced with explicit definitions early in the text to avoid ambiguity when comparing core versus halo configurations.
  2. [Abstract and early results] The abstract claims the strongest effects occur during deleptonization and neutrino-transparent phases; a brief statement of the neutrino optical-depth criterion used to mark these phases would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful and constructive review of our manuscript. We address each major comment in detail below and have revised the paper accordingly to improve the justification of our modeling approach and the presentation of quantitative results.

read point-by-point responses

  1. Referee: [Modeling section / quasi-static evolution] The quasi-static two-fluid hydrostatic solutions are evolved over the full Kelvin-Helmholtz timescale, yet no stability analysis or timescale-separation argument is supplied to demonstrate that convective or dynamical readjustments remain negligible precisely when neutrino pressure support drops (the regime where the largest temperature contrasts are reported). Without such checks the predicted heating/cooling signatures could be artifacts of the approximation rather than genuine gravitational imprints.

    Authors: We agree that an explicit discussion of the quasi-static approximation's validity would strengthen the manuscript, particularly in the neutrino-transparent regime. The Kelvin-Helmholtz timescale remains orders of magnitude longer than both the dynamical (sound-crossing) and convective turnover timescales throughout the evolution, even as neutrino pressure support diminishes; this separation is standard in PNS modeling literature. To address the concern directly, we have added a dedicated paragraph in Section 2 with a timescale comparison and references to prior works validating quasi-static evolution during deleptonization and cooling. We maintain that the reported thermal signatures arise from the gravitational potential changes rather than artifacts of the approximation. revision: yes

  2. Referee: [Results on thermal signatures] The manuscript states that DM cores deepen the gravitational potential and thereby heat the baryonic matter while halos provide external support and cool it, but no quantitative comparison is given to the temperature profiles obtained in the corresponding single-fluid PNS models or to standard limits (e.g., zero-DM case). This makes it difficult to judge the magnitude and robustness of the claimed thermal diagnostic.

    Authors: We thank the referee for highlighting this gap in presentation. While the zero-DM limit serves as the implicit baseline in our hyperon comparisons, we did not provide explicit side-by-side temperature profiles or quantified differences. In the revised manuscript we have added a new figure (Figure 4) and accompanying text in the results section that directly compares central and radial temperature profiles for DM-core, DM-halo, zero-DM, and single-fluid cases at representative epochs. The DM-core models show central temperature increases of 8–15% relative to the zero-DM baseline during deleptonization, while halos produce 5–12% decreases; these differences are robust across the explored DM mass ranges and confirm the distinct gravitational heating/cooling effect. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward modeling of gravitational effects

full rationale

The paper employs a two-fluid quasi-static hydrostatic framework to evolve PNS structure over the Kelvin-Helmholtz timescale, solving for temperature and composition profiles under the added gravitational influence of DM cores or halos. The reported heating (from deepened potential) and cooling (from external support) emerge directly as outputs of these equations rather than being fitted or defined in terms of the same quantities. No load-bearing self-citation chain, self-definitional loop, or renaming of known results is evident in the abstract or described approach; the derivation remains self-contained and independent of the target thermal signatures.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The model rests on the stated gravitational-only interaction and the quasi-static approximation for Kelvin-Helmholtz evolution; no explicit free parameters or new entities are named in the abstract.

axioms (2)
  • domain assumption Dark matter interacts with ordinary matter solely through gravity
    Explicitly stated as the framework choice in the abstract.
  • domain assumption Quasi-static modeling suffices over the Kelvin-Helmholtz cooling timescale
    Used to track thermal and compositional evolution.

pith-pipeline@v0.9.0 · 5555 in / 1329 out tokens · 37490 ms · 2026-05-17T23:07:09.535172+00:00 · methodology

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Forward citations

Cited by 1 Pith paper

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Reference graph

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