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arxiv: 2512.14838 · v2 · submitted 2025-12-16 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

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Non-Thermal Production of Sexaquark Dark Matter

Marianne Moore (MIT) , Stefano Profumo (UCSC)
Authors on Pith no claims yet

Pith reviewed 2026-05-16 21:36 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE
keywords sexaquarkdark matternon-thermal productionreheatoncoalescenceQCD scaleearly universe
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The pith

Non-thermal production from late-decaying reheatons can match the observed sexaquark dark matter density.

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

Standard thermal freeze-out predicts a sexaquark abundance many orders of magnitude below the observed dark matter density, and thermal production may never occur if the maximum post-inflation temperature stays below the QCD scale. Late-decaying reheatons provide a non-thermal channel by injecting strange-quark-rich matter that coalesces into sexaquarks. The final relic density is set by the reheaton branching fraction into strange matter and the coalescence probability during the matter-dominated or early radiation-dominated epoch. Compact expressions for this abundance are given for reheating temperatures between 10 and 100 MeV with reheaton masses above the QCD confinement scale. The mechanism respects collider, precision, and indirect detection constraints while establishing non-thermal production as a viable pathway.

Core claim

Using late-decaying reheatons as a representative case, the final abundance is determined by two quantities: the branching fraction into strange-quark-rich matter and the coalescence probability into sexaquarks during the matter-dominated or early radiation-dominated epoch. Compact expressions and benchmark calculations are provided for reheating temperatures TR in [10, 100] MeV and reheaton masses above the QCD confinement scale. Unlike the predictive but unsuccessful thermal scenario, non-thermal production is sensitive to injection microphysics, coalescence efficiency, and residual entropy dilution. The results establish non-thermal production as a viable pathway to sexaquark dark matter.

What carries the argument

Late-decaying reheatons that produce strange-quark-rich matter which coalesces into uuddss sexaquarks.

Load-bearing premise

Representative values for the branching fraction into strange-quark-rich matter and the coalescence probability can be chosen to reach the observed dark matter density without violating collider or indirect detection bounds, assuming reheatons above the QCD scale exist and decay in the required epoch.

What would settle it

A collider or indirect detection measurement that finds no residual antisexaquarks or places the sexaquark abundance outside the range allowed by viable branching fractions and coalescence probabilities.

Figures

Figures reproduced from arXiv: 2512.14838 by Marianne Moore (MIT), Stefano Profumo (UCSC).

Figure 2
Figure 2. Figure 2: Branching ratios as a function of the reheaton mass ϕ from Eqs. (9) (Yukawa scalar in orange and pseudoscalar in yellow) and (18) (flavor￾universal Z ′ vector in magenta and axial-vector in violet). The thresholds for the reheaton to decay into two charm quarks (2mc) and two bottom quarks (2mb) are illustrated. into a compact, long-lived S. The efficiency of sexaquark production from reheaton decay is then… view at source ↗
Figure 3
Figure 3. Figure 3: Fraction fS of reheaton decay producing sexaquarks as a function of the reheaton mass. The grey band indicates the region where the full dark matter abundance in sexaquarks can be obtained for the reheating temperature range considered throughout this work, 10 ≤ TR ≤ 100 MeV, with smaller reheating temperatures corresponding to the top of the band. The colored bands indicate the range obtained for two scen… view at source ↗
read the original abstract

Standard thermal freeze-out scenarios with QCD-scale interaction rates predict a $uuddss$ sexaquark relic abundance many orders of magnitude below the observed dark matter density, representing a key challenge for sexaquark dark matter models. Additionally, if the maximum post-inflationary temperature never exceeds the QCD confinement scale, the usual thermal/chemical-equilibrium production of the sexaquark near $T \sim T_{\rm QCD} \simeq 150 - 170$ MeV never occurs. In this work we show that non-thermal mechanisms can naturally overcome this obstacle. Using late-decaying reheatons as a representative case (while noting the broader applicability), we demonstrate that the final abundance is determined by two quantities: the branching fraction into strange-quark-rich matter and the coalescence probability into sexaquarks during the matter-dominated or early radiation-dominated epoch. We provide compact expressions and benchmark calculations for reheating temperatures $T_R \in [10, 100]$ MeV and reheaton masses above the QCD confinement scale. Unlike the predictive but unsuccessful thermal scenario, non-thermal production is sensitive to injection microphysics, coalescence efficiency, and residual entropy dilution. We delineate the viable parameter space, evaluate collider and precision constraints on representative reheaton models, and derive indirect detection bounds on residual antisexaquark populations. Our results establish non-thermal production as a viable pathway to sexaquark dark matter and highlight broader implications for non-equilibrium mechanisms in the early universe.

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 paper claims that non-thermal production via late-decaying reheatons (m > QCD scale) can overcome the underproduction of uuddss sexaquark dark matter in thermal scenarios. The final abundance is determined by two quantities—the branching fraction B into strange-quark-rich matter and the coalescence probability P—during matter- or early radiation-dominated epochs, with compact expressions and benchmark calculations provided for TR in [10, 100] MeV. The work delineates viable (B, P) parameter space after evaluating collider, precision, and indirect-detection constraints, establishing non-thermal injection as a viable pathway.

Significance. If the viable space is shown to be non-empty with robust derivations, the result supplies a concrete alternative to thermal freeze-out for sexaquark DM and illustrates how non-equilibrium mechanisms can set relic densities when thermal production is suppressed. The compact expressions for specific TR values and explicit treatment of entropy dilution are strengths that could aid model-building.

major comments (3)
  1. [Section 4] The central viability claim rests on the existence of (B, P) pairs that simultaneously reproduce the observed DM density and satisfy all bounds, yet the manuscript provides only representative benchmark calculations without full numerical scans or error propagation; it is therefore unclear whether the minimum B required for the observed abundance lies below the maximum B permitted by collider/precision constraints for any reheaton mass above the QCD scale.
  2. [Section 3] The compact expressions for the sexaquark yield (presumably derived from the Boltzmann equation in the matter- or early radiation-dominated epoch) are stated without the intermediate steps, approximation conditions, or dependence on the reheaton lifetime and decay width; this makes it impossible to assess whether additional factors (e.g., entropy dilution or residual thermal contributions) have been correctly omitted.
  3. [Section 6] Indirect-detection bounds on residual antisexaquark populations are derived using annihilation cross sections that appear chosen independently of the non-thermal production channel; a consistency check is needed to confirm that the same coalescence probability P used for production does not alter the late-time annihilation rate in a way that tightens the bounds beyond the quoted limits.
minor comments (2)
  1. [Abstract] Notation for reheating temperature alternates between T_R and TR; adopt a single symbol throughout.
  2. [Introduction] The definition of the reheaton as a generic late-decaying particle should be stated explicitly in the introduction rather than introduced only via the example.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comments. We address each major comment point by point below, indicating the revisions we plan to incorporate.

read point-by-point responses

  1. Referee: [Section 4] The central viability claim rests on the existence of (B, P) pairs that simultaneously reproduce the observed DM density and satisfy all bounds, yet the manuscript provides only representative benchmark calculations without full numerical scans or error propagation; it is therefore unclear whether the minimum B required for the observed abundance lies below the maximum B permitted by collider/precision constraints for any reheaton mass above the QCD scale.

    Authors: We agree that benchmark calculations alone leave the full extent of the viable parameter space unclear. In the revised manuscript we will add a numerical scan over reheaton masses above the QCD scale, sampling B and P in physically allowed ranges with propagated uncertainties from coalescence probabilities, to explicitly map the regions where the B needed for the observed abundance lies below collider and precision upper limits. revision: yes

  2. Referee: [Section 3] The compact expressions for the sexaquark yield (presumably derived from the Boltzmann equation in the matter- or early radiation-dominated epoch) are stated without the intermediate steps, approximation conditions, or dependence on the reheaton lifetime and decay width; this makes it impossible to assess whether additional factors (e.g., entropy dilution or residual thermal contributions) have been correctly omitted.

    Authors: The expressions follow from integrating the Boltzmann equation for non-thermal injection under the approximation that reheaton decay occurs in a matter- or early radiation-dominated epoch with lifetime much longer than the Hubble time at T_R. We will add an appendix containing the full derivation, the explicit dependence on the decay width, the validity conditions, and confirmation that entropy dilution is included via the standard scale-factor evolution while residual thermal production is absent because the maximum temperature remains below the QCD scale. revision: yes

  3. Referee: [Section 6] Indirect-detection bounds on residual antisexaquark populations are derived using annihilation cross sections that appear chosen independently of the non-thermal production channel; a consistency check is needed to confirm that the same coalescence probability P used for production does not alter the late-time annihilation rate in a way that tightens the bounds beyond the quoted limits.

    Authors: The coalescence probability P controls formation efficiency only during the early non-thermal production epoch and does not enter the late-time annihilation cross section, which is fixed by the intrinsic low-velocity properties of the sexaquark. We will insert an explicit consistency check showing that the quoted indirect-detection bounds are unaffected by the value of P, as the annihilation rate depends solely on the present-day number density and velocity-averaged cross section. revision: partial

Circularity Check

0 steps flagged

No circularity: abundance parameterized by independent inputs B and P

full rationale

The derivation expresses final sexaquark yield via two explicit input parameters (branching fraction into strange-quark-rich matter and coalescence probability) whose values are chosen to match the observed density while satisfying external collider/precision/indirect bounds. Compact expressions for TR = 10-100 MeV are given in terms of these inputs, with viable space delineated by evaluating constraints on representative reheaton models. No step reduces by construction to a fitted quantity renamed as prediction, no self-citation chain bears the central claim, and no ansatz or uniqueness theorem is smuggled in. The analysis is a standard parameter-space viability study whose central result (existence of allowed (B,P) region) is falsifiable against the listed bounds and does not tautologically reproduce its inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 1 invented entities

The central claim rests on two free parameters that control the final abundance and on standard cosmological assumptions about reheating epochs; the reheaton itself is introduced as a representative mechanism.

free parameters (2)
  • branching fraction into strange-quark-rich matter
    Controls the fraction of reheaton decays that produce the strange quarks needed for sexaquark formation.
  • coalescence probability into sexaquarks
    Determines the efficiency with which injected strange quarks form bound sexaquarks during the relevant epoch.
axioms (2)
  • domain assumption Late-decaying reheatons exist with masses above the QCD confinement scale and decay during a matter-dominated or early radiation-dominated epoch.
    Representative case used to model non-thermal injection after inflation.
  • standard math QCD confinement scale lies between 150 and 170 MeV.
    Standard input from particle physics used to define the temperature window.
invented entities (1)
  • reheaton no independent evidence
    purpose: Late-decaying particle that injects strange quarks non-thermally after the QCD scale.
    Introduced as a representative mechanism to enable the non-thermal pathway; no independent detection signature is derived beyond general constraints.

pith-pipeline@v0.9.0 · 5568 in / 1725 out tokens · 72941 ms · 2026-05-16T21:36:34.392652+00:00 · methodology

discussion (0)

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Reference graph

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