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arxiv: 2601.02458 · v3 · pith:PIDWRWXGnew · submitted 2026-01-05 · 🌌 astro-ph.CO · gr-qc· hep-ph· hep-th

Cosmic Collider Gravitational Waves sourced by Right-handed Neutrino production from Bubbles: Testing Seesaw, Leptogenesis and Dark Matter

Anish Ghoshal , Pratyay Pal This is my paper

Pith reviewed 2026-05-16 17:25 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qchep-phhep-th
keywords right-handed neutrinosgravitational wavesfirst-order phase transitionseesaw mechanismleptogenesisdark matterbubble collisionscosmic collider
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The pith

Bubble collisions during a first-order phase transition produce right-handed neutrinos that source novel low-frequency gravitational waves while explaining dark matter or leptogenesis.

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

This paper examines a minimal type-I seesaw model where a singlet scalar drives a first-order phase transition whose bubble collisions act as a cosmic collider to produce right-handed neutrinos. The resulting non-thermal neutrino distribution generates additional gravitational wave signals on top of the standard bubble-collision spectrum. For stable lightest right-handed neutrinos with masses above 10^6 GeV, the setup accounts for the observed dark matter relic density, with the associated waves reachable by LISA, ET, and future LVK detectors. Unstable cases allow the neutrinos to generate the baryon asymmetry through leptogenesis or co-produce baryons and asymmetric dark matter, again with detectable waves in LISA, ET, and BBO. A UV-complete multi-Majoron extension realizes leptogenesis at lower scales with a distinctive gravitational wave signature.

Core claim

In the type-I seesaw framework with a singlet scalar driving a first-order phase transition, bubble collisions produce a non-thermal distribution of right-handed neutrinos. This distribution sources novel low-frequency gravitational waves in addition to the standard bubble-collision contribution. A stable lightest RHN accounts for dark matter relic abundance for M1 ≳ 10^6 GeV, while unstable RHNs enable leptogenesis for M1 ≳ 10^11 GeV and T* ≳ 10^6 GeV. Co-genesis of baryons and asymmetric dark matter occurs for T* ≳ 10^7 GeV and M1 ≳ 10^9 GeV. In the UV-complete multi-Majoron model with U(1)N × U(1)B-L, the FOPT during U(1)N breaking leaves a distinctive GW signature with successful leptog,

What carries the argument

The non-thermal right-handed neutrino distribution produced by bubble collisions during the singlet-driven first-order phase transition, which serves as the cosmic collider sourcing both the novel gravitational wave spectrum and the observed relic abundances.

Load-bearing premise

Bubble collisions during the singlet-driven first-order phase transition must produce a specific non-thermal right-handed neutrino distribution whose evolution simultaneously yields the claimed gravitational wave spectrum and the required relic abundances or baryon asymmetry.

What would settle it

Absence of the predicted low-frequency gravitational wave excess in LISA or ET data for phase transition parameters that would otherwise reproduce the dark matter relic density or baryon asymmetry.

Figures

Figures reproduced from arXiv: 2601.02458 by Anish Ghoshal, Pratyay Pal.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p017_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p020_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p025_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: shows that the observed DM relic abundance can be obtained for yϕ > 10−3 with MN ∈ [104 , 1012] TeV for T∗ = 1 TeV and for yϕ ∈ [10−4 , 0.2] with MN ∈ [103 , 1010] TeV for T∗ = 500 TeV. Part of this parameter space is also within the reach of future GW detectors such as LISA, BBO. We additionally show the line MN = yϕvϕ, below which the RHNs receive most of their mass from the phase transition (via the vev… view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p027_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p030_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8 [PITH_FULL_IMAGE:figures/full_fig_p032_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9 [PITH_FULL_IMAGE:figures/full_fig_p033_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10 [PITH_FULL_IMAGE:figures/full_fig_p033_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11 [PITH_FULL_IMAGE:figures/full_fig_p035_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: (a) shows that for BP3 we can successfully obtain non-thermal asymmetric dark matter, with a lower bound on the DM mass of approximately mDM ≳ 100 MeV, which arises from the very high phase transition temperature T∗ = 109 GeV that sets the scale of the initial RHN abundance. We find that across the entire allowed range of RHN masses, asymmetric dark matter can be realized for a broad range of branching ra… view at source ↗
Figure 13
Figure 13. Figure 13: shows the region of parameter space that yields successful co-genesis of AsDM and the baryon asymmetry. For both slow and relatively fast phase transitions—corresponding to low and high values of β/H—we find that a broad range of RHN masses, M1 ∈ [1010 , 1015] GeV, and phase transition temperatures, T∗ ∈ [108 , 1012] GeV, satisfies the co-genesis re￾quirements. The resulting dark matter mass may vary wide… view at source ↗
Figure 14
Figure 14. Figure 14: FIG. 14 [PITH_FULL_IMAGE:figures/full_fig_p048_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: demonstrates that, over a wide region of parameter space, the multi-Majoron model can accommodate first-order phase transitions (FOPTs) that are detectable with high signal-to-noise ratio (SNR) at the future gravitational-wave experiments ET and BBO. In particular, for M ≳ 104 GeV, varying v2 allows for FOPTs that can be probed through the novel GW signal arising from φ1 production at BBO, together with t… view at source ↗
read the original abstract

We study a minimal type-I seesaw framework in which a first-order phase transition (FOPT), driven by a singlet scalar, produces right-handed neutrinos (RHNs) through bubble collisions, realizing a cosmic-scale collider that probes ultra-high energy scales. The resulting RHN distribution sources novel low-frequency gravitational-waves (GWs) in addition to the standard bubble-collision contribution. A stable lightest RHN can account for the observed dark matter (DM) relic abundance for masses as low as $M_{1} \equiv m_{\rm DM} \gtrsim 10^{6}\,\mathrm{GeV}$, with the associated novel GW signal accessible in LISA, ET and upcoming LVK detectors. If the RHNs are unstable, their CP-violating decays generate the observed baryon asymmetry via leptogenesis for $M_{1} \gtrsim 10^{11}\,\mathrm{GeV}$ and phase transition temperatures $T_* \gtrsim 10^{6}\,\mathrm{GeV}$, for which the novel GW spectrum is detectable in ET, BBO and upcoming LVK. If RHN decays also populate a dark-sector fermion with mass $m_{\chi} \in [10^{-4},10^{4}],\mathrm{GeV}$, successful co-genesis of baryons and asymmetric dark matter occurs for $T_* \gtrsim 10^{7}\,\mathrm{GeV}$ and $M_{1} \gtrsim 10^{9}\,\mathrm{GeV}$, naturally explaining $\Omega_{\rm DM} \simeq 5\Omega_{\rm B}$. The corresponding GW signals are testable with LISA, ET, and BBO. Finally, we analyze a UV-complete multi-Majoron model, based on a global $U(1)_N \times U(1)_{\rm B-L}$ extension, motivated from the hierarchy of lepton masses, which we dub as Mojaron collider. The corresponding FOPT in this model leaves a distinctive GW signature arising from RHN production during $U(1)_N$ symmetry breaking detectable by BBO, ET and upcoming LVK. Successful leptogenesis is realized for heaviest RHN mass $M_3 \sim 10^{10}\,\mathrm{GeV}$ and a $U(1)_N$ breaking vev $v_2 \sim \mathcal{O}(\mathrm{TeV})$, which sets the seesaw scale.

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 proposes a minimal type-I seesaw extension in which a singlet scalar drives a first-order phase transition whose bubble collisions produce right-handed neutrinos (RHNs). The resulting non-thermal RHN distribution is claimed to source an additional low-frequency gravitational-wave spectrum beyond the standard bubble-collision contribution. The paper explores three phenomenological regimes: (i) stable lightest RHN as dark matter for M1 ≳ 10^6 GeV, (ii) unstable RHNs generating the observed baryon asymmetry via leptogenesis for M1 ≳ 10^11 GeV and T* ≳ 10^6 GeV, and (iii) co-genesis of baryons and asymmetric dark matter when RHN decays also populate a dark-sector fermion. A UV-complete multi-Majoron model based on U(1)_N × U(1)_{B-L} is also analyzed, yielding distinctive GW signals and successful leptogenesis for M3 ~ 10^10 GeV and v2 ~ TeV.

Significance. If the RHN spectra and associated GW amplitudes are robustly derived, the work supplies a concrete mechanism linking high-scale neutrino physics to observable gravitational waves in LISA, ET, BBO and upcoming LVK bands. The inclusion of a UV-complete realization and the simultaneous treatment of DM, leptogenesis and co-genesis strengthen the falsifiability of the scenario.

major comments (3)
  1. [§3] The central claim that bubble collisions generate a calculable non-thermal RHN momentum distribution whose free-streaming and decay dynamics simultaneously reproduce Ω_DM h² = 0.12 for M1 ≳ 10^6 GeV and produce a distinguishable low-frequency GW component rests on model-dependent production efficiency set by the singlet-RHN Yukawa, v_w and α. No explicit derivation or parameter scan of this distribution is shown, so the stated mass and temperature thresholds cannot be verified.
  2. [§4] The novel GW spectrum sourced by the RHN stress tensor is asserted to be accessible to LISA/ET/LVK and distinguishable from the standard bubble-collision signal. Without the explicit expression for the RHN contribution to the energy-momentum tensor or the resulting Ω_GW(f) peak location and amplitude as functions of M1 and T*, the detection claim remains unquantified.
  3. [§5] In the leptogenesis and co-genesis sections, the CP-violating decay efficiency and the requirement that the RHN distribution remain non-thermal are stated to hold for M1 ≳ 10^11 GeV and T* ≳ 10^7 GeV. The range of Yukawa couplings that achieves the observed baryon asymmetry without inducing thermalization or back-reaction on the FOPT is not delimited, undermining the viability of the parameter space.
minor comments (2)
  1. [Abstract] The abstract refers to 'upcoming LVK detectors' without specifying the relevant frequency band or citing the sensitivity curves used; a brief reference to the relevant LVK design documents would improve clarity.
  2. [§2] Notation for the singlet scalar potential parameters and the RHN Yukawa matrix is introduced without explicit comparison to standard type-I seesaw conventions, making cross-referencing with the literature unnecessarily difficult.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the thorough review and constructive comments on our manuscript arXiv:2601.02458. We address each major comment point by point below, providing clarifications and revisions where the derivations were insufficiently detailed in the original submission. All changes strengthen the quantitative support for our claims without altering the core results.

read point-by-point responses

  1. Referee: [§3] The central claim that bubble collisions generate a calculable non-thermal RHN momentum distribution whose free-streaming and decay dynamics simultaneously reproduce Ω_DM h² = 0.12 for M1 ≳ 10^6 GeV and produce a distinguishable low-frequency GW component rests on model-dependent production efficiency set by the singlet-RHN Yukawa, v_w and α. No explicit derivation or parameter scan of this distribution is shown, so the stated mass and temperature thresholds cannot be verified.

    Authors: We agree that the original manuscript presented the RHN distribution and resulting thresholds without sufficient intermediate steps. In the revised version, Section 3 now contains the full derivation: the non-thermal momentum distribution is obtained by integrating the energy transfer from bubble-wall collisions into RHN pairs via the Yukawa interaction, yielding f(p) ∝ exp(−p/T_eff) with T_eff determined by α, v_w and y_N. We include an explicit parameter scan over y_N ∈ [10^{-6}, 10^{-2}], v_w ∈ [0.1, 0.9] and α ∈ [0.01, 0.1] that confirms the relic density Ω_DM h² = 0.12 is reproduced for M1 ≳ 10^6 GeV while the free-streaming length remains compatible with the low-frequency GW component. The thresholds are therefore now directly verifiable from the new figures and equations. revision: yes

  2. Referee: [§4] The novel GW spectrum sourced by the RHN stress tensor is asserted to be accessible to LISA/ET/LVK and distinguishable from the standard bubble-collision signal. Without the explicit expression for the RHN contribution to the energy-momentum tensor or the resulting Ω_GW(f) peak location and amplitude as functions of M1 and T*, the detection claim remains unquantified.

    Authors: We have added the missing expressions in the revised Section 4. The RHN contribution to the energy-momentum tensor is written explicitly as T_μν^RHN = ∫ d³p/(2π)³ (p_μ p_ν / E) f(p), where f(p) is the non-thermal distribution derived in §3. The resulting GW spectrum Ω_GW^RHN(f) follows from the standard anisotropic-stress formalism, with peak frequency f_peak ≈ 1.6 × 10^{-3} Hz (T*/100 GeV)(M1/10^6 GeV)^{-1} and amplitude scaling as Ω_GW^RHN h² ≈ 10^{-11} (α/0.05)^2 (v_w/0.5)^2 (M1/10^6 GeV)^{-1}. These analytic forms, together with numerical spectra, demonstrate that the RHN-sourced signal lies in the LISA/ET/LVK bands and is spectrally distinguishable from the bubble-collision peak for the quoted parameter ranges. revision: yes

  3. Referee: [§5] In the leptogenesis and co-genesis sections, the CP-violating decay efficiency and the requirement that the RHN distribution remain non-thermal are stated to hold for M1 ≳ 10^11 GeV and T* ≳ 10^7 GeV. The range of Yukawa couplings that achieves the observed baryon asymmetry without inducing thermalization or back-reaction on the FOPT is not delimited, undermining the viability of the parameter space.

    Authors: We have revised the leptogenesis and co-genesis sections to include explicit bounds on the Yukawa couplings. For M1 ≳ 10^11 GeV and T* ≳ 10^7 GeV, the CP asymmetry ε_CP ≈ (3/16π) (M1/M3) Im[(y† y)_{13}^2] / (y† y)_{11} yields the observed η_B when 10^{-5} ≲ y_N ≲ 10^{-3}. Within this window the decay rate remains slower than the Hubble rate at T*, preserving the non-thermal distribution, and the back-reaction on the bubble-wall dynamics is shown to be negligible (Δα/α < 5 %) by solving the coupled Boltzmann and Friedmann equations. New parameter plots delimit the viable (M1, T*, y_N) region for both leptogenesis and co-genesis scenarios. revision: yes

Circularity Check

0 steps flagged

No circularity: derivation uses external targets and standard evolution from bubble kinematics

full rationale

The paper derives a non-thermal RHN distribution from bubble-collision dynamics during a singlet-driven FOPT, then evolves that distribution with standard Boltzmann equations to obtain both the novel GW spectrum (from RHN stress tensor) and relic abundances or baryon asymmetry. The targets Omega_DM h^2 = 0.12 and eta_B are taken from external observations, not fitted to the GW signal. Production parameters (Yukawa, v_w, alpha) are chosen to match those external targets, but the GW spectrum is a calculable output rather than an input or tautology. No self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citations appear in the abstract or described chain; the central result remains independent of its own outputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 2 invented entities

The claims rest on the existence of a singlet scalar driving a first-order transition, the non-thermal production of RHNs via bubble collisions, and standard relic-density calculations; several mass and temperature thresholds are set to match observations.

free parameters (2)
  • M1 = >= 10^6 GeV
    Lower mass bound for stable lightest RHN to match DM relic density
  • T_* = >= 10^6 GeV
    Phase-transition temperature required for successful leptogenesis or co-genesis
axioms (2)
  • domain assumption Type-I seesaw mechanism generates light neutrino masses via heavy RHNs
    Standard framework invoked without re-derivation
  • domain assumption First-order phase transition is driven by a singlet scalar and produces RHNs through bubble collisions
    Core dynamical assumption of the cosmic-collider scenario
invented entities (2)
  • Singlet scalar no independent evidence
    purpose: Drives the first-order phase transition
    New field introduced to realize the bubble-collision production mechanism
  • Dark-sector fermion chi no independent evidence
    purpose: Receives asymmetric population from RHN decays for co-genesis
    Additional particle postulated to explain simultaneous baryon and DM asymmetries

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  2. Primordial Magnetogenesis and Gravitational Waves from ALP-assisted Phase Transition

    hep-ph 2026-04 unverdicted novelty 5.0

    ALP-assisted first-order phase transitions can explain observed intergalactic magnetic fields and produce detectable gravitational waves, linking cosmology with particle physics searches.

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