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arxiv: 2605.15289 · v1 · submitted 2026-05-14 · 🌌 astro-ph.HE · hep-ph

Ultra high-energy cosmic rays from relativistic outflows in accretion induced collapse of white dwarfs

Mainak Mukhopadhyay , Shunsaku Horiuchi This is my paper

Pith reviewed 2026-05-19 16:07 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-ph
keywords ultra-high-energy cosmic raysaccretion-induced collapsewhite dwarfsrelativistic outflowsheavy nucleiprotomagnetarUHECR sourcescosmic ray acceleration
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The pith

Relativistic outflows from accretion-induced white dwarf collapses can dominantly power the observed ultra-high-energy cosmic rays.

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

The paper argues that when a white dwarf accretes mass and spins up to the Chandrasekhar limit while strongly magnetized, it collapses to a protomagnetar. This collapse launches a low-entropy, magnetically dominated relativistic outflow that forms and accelerates heavy nuclei to ultra-high energies. If a majority of such events produce these outflows, the total energy released in ultra-high-energy cosmic rays falls in the range of a few 10^43 to 10^45 erg per cubic megaparsec per year, enough to explain the observed flux. This mechanism supplies a new candidate source for particles whose origins remain uncertain. Uncertainties in collapse rates and acceleration efficiency still permit the contribution to match data when iron-like nuclei are assumed.

Core claim

Accretion-induced collapse of rapidly rotating, highly magnetized white dwarfs forms a protomagnetar that drives a magnetically dominated relativistic outflow. The low entropy in this outflow enables efficient formation of heavy nuclei, which are then accelerated to ultra-high energies. The resulting energy generation rate density reaches a few 10^43 to 10^45 erg Mpc^{-3} yr^{-1}, sufficient to account for observed ultra-high-energy cosmic rays if a majority of collapses host such outflows and nuclei are iron-like.

What carries the argument

Magnetically dominated relativistic outflows launched by protomagnetars formed in accretion-induced collapse, which carry low entropy to enable efficient heavy-nuclei acceleration to ultra-high energies.

If this is right

  • If most accretion-induced collapses launch relativistic outflows, these events can supply the full observed ultra-high-energy cosmic ray energy budget.
  • The mechanism naturally produces a heavy-nuclei composition at the highest energies.
  • The calculated energy generation rate density remains compatible with observations after folding in current uncertainties on rates and acceleration efficiency.
  • Ultra-high-energy cosmic rays from this channel would arrive from sources distributed according to the local rate of white-dwarf accretion events.

Where Pith is reading between the lines

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

  • Future radio or optical surveys that tighten the local rate of accretion-induced collapses could directly test whether enough events occur to dominate the ultra-high-energy cosmic ray flux.
  • If confirmed, this source class would link the origin of ultra-high-energy cosmic rays to the formation channel of some neutron stars and magnetars.
  • Heavy-nuclei acceleration in these outflows could produce distinct secondary neutrino or gamma-ray signatures detectable by current observatories.

Load-bearing premise

A majority of accretion-induced collapses must produce relativistic outflows capable of efficiently accelerating heavy nuclei to ultra-high energies.

What would settle it

Direct measurement of the accretion-induced collapse rate in the local universe that falls well below the value needed to supply the required energy generation rate density, or composition data showing ultra-high-energy cosmic rays are not dominated by iron-like nuclei.

Figures

Figures reproduced from arXiv: 2605.15289 by Mainak Mukhopadhyay, Shunsaku Horiuchi.

Figure 1
Figure 1. Figure 1: FIG. 1. AICs as sources of observed UHECRs on the charac [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Time evolution of the magnetization [PITH_FULL_IMAGE:figures/full_fig_p002_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Time evolution of the comoving maximum CR energy [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. The contribution of jets originating from AIC of WDs [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
read the original abstract

When a rapidly-rotating, highly magnetized white dwarf (WD) approaches the Chandrashekhar limit through mass accretion, it can undergo an accretion-induced collapse (AIC) to form a proto-neutron star or protomagnetar. The protomagnetar can drive a magnetically-dominated relativistic outflow, whose low entropy can lead to efficient formation of heavy nuclei. In this work, we propose that such relativistic outflows from AIC of WDs can contribute as sources of ultra high-energy cosmic rays (UHECRs). We model the acceleration of heavy nuclei in these relativistic outflows, and show that AICs can dominantly power the observed UHECRs, if a majority of them host relativistic outflows. Accounting for uncertainties in the acceleration mechanisms and AIC rates, AICs can contribute $\sim$ a few $10^{43} - 10^{45}\ {\rm erg \ Mpc}^{-3} {\rm yr}^{-1}$ in UHECR energy generation rate density, assuming iron-like nuclei.

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 paper proposes that accretion-induced collapse (AIC) of rapidly rotating, highly magnetized white dwarfs can produce protomagnetars driving magnetically dominated relativistic outflows. These outflows, with low entropy, enable efficient formation and acceleration of heavy (iron-like) nuclei to ultra-high energies. The central claim is that if a majority of AIC events host such outflows, they can dominantly account for the observed UHECR flux, contributing an energy generation rate density of roughly a few 10^{43}–10^{45} erg Mpc^{-3} yr^{-1} after folding in uncertainties on AIC rates and acceleration efficiencies.

Significance. If the modeling assumptions hold, this work identifies a new potential class of UHECR sources tied to binary evolution and protomagnetar formation, offering a mechanism that naturally favors heavy nuclei. The linkage between AIC rates, relativistic outflow dynamics, and cosmic-ray acceleration is a useful addition to the literature on UHECR origins. However, the result is framed as a consistency check rather than a sharp prediction, limiting its immediate impact on resolving the UHECR source problem.

major comments (2)
  1. [Abstract] Abstract: The statement that AICs 'can dominantly power the observed UHECRs' rests on the assumption that a majority of AIC events produce relativistic outflows capable of efficient heavy-nuclei acceleration. No independent constraint (e.g., from binary population synthesis or magnetar birth-rate statistics) is provided for this fraction; the quoted energy-generation interval is obtained by varying the outflow-hosting fraction and acceleration efficiency within broad uncertainties, rendering the match to the observed flux a consistency check rather than a model-derived result.
  2. [Main text (energy generation rate section)] The energy generation rate density range (a few 10^{43}–10^{45} erg Mpc^{-3} yr^{-1}) is presented as accounting for uncertainties, but the load-bearing step—deriving the contribution from the product of AIC rate density, outflow fraction, and acceleration efficiency—lacks a quantitative sensitivity analysis showing how the result changes when the outflow fraction is fixed to observationally motivated values below 50%.
minor comments (2)
  1. [Acceleration model] Clarify the precise definition of 'iron-like nuclei' and the assumed charge and mass numbers used in the acceleration calculation.
  2. [Introduction] The abstract and introduction would benefit from a brief comparison to existing UHECR source models (e.g., GRBs or AGN) to better situate the novelty of the AIC channel.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for the constructive and detailed review of our manuscript. We agree that the results are best viewed as a consistency check under specific assumptions about the outflow fraction and have revised the text to clarify this framing while adding the requested sensitivity analysis.

read point-by-point responses

  1. Referee: [Abstract] The statement that AICs 'can dominantly power the observed UHECRs' rests on the assumption that a majority of AIC events produce relativistic outflows capable of efficient heavy-nuclei acceleration. No independent constraint (e.g., from binary population synthesis or magnetar birth-rate statistics) is provided for this fraction; the quoted energy-generation interval is obtained by varying the outflow-hosting fraction and acceleration efficiency within broad uncertainties, rendering the match to the observed flux a consistency check rather than a model-derived result.

    Authors: We agree that the result constitutes a consistency check rather than a sharp, model-derived prediction, since it depends on the fraction of AIC events that produce relativistic outflows. The manuscript explores plausible parameter ranges within existing uncertainties on rates and efficiencies to identify conditions under which AIC outflows could contribute substantially to the UHECR flux. We will revise the abstract to more explicitly state the conditional nature of the claim and to avoid any implication of definitive dominance without supporting constraints on the fraction. Deriving new independent constraints from binary population synthesis or magnetar statistics lies outside the scope of this work, which centers on modeling the relativistic outflows and heavy-nuclei acceleration. revision: partial

  2. Referee: [Main text (energy generation rate section)] The energy generation rate density range (a few 10^{43}–10^{45} erg Mpc^{-3} yr^{-1}) is presented as accounting for uncertainties, but the load-bearing step—deriving the contribution from the product of AIC rate density, outflow fraction, and acceleration efficiency—lacks a quantitative sensitivity analysis showing how the result changes when the outflow fraction is fixed to observationally motivated values below 50%.

    Authors: We acknowledge that an explicit sensitivity analysis would improve the presentation. In the revised manuscript we will add a quantitative discussion, including a figure or table, that shows the UHECR energy generation rate density as a function of the outflow-hosting fraction. This will explicitly illustrate the scaling for fractions below 50% and clarify the minimum fraction required for AICs to remain a significant contributor under conservative assumptions. revision: yes

standing simulated objections not resolved
  • Providing independent constraints on the fraction of AIC events hosting relativistic outflows from binary population synthesis or magnetar birth-rate statistics.

Circularity Check

1 steps flagged

UHECR energy generation rate range from AICs overlaps observations by varying outflow-hosting fraction and acceleration efficiency within uncertainties

specific steps
  1. fitted input called prediction [Abstract]
    "Accounting for uncertainties in the acceleration mechanisms and AIC rates, AICs can contribute ∼ a few 10^{43} - 10^{45} erg Mpc^{-3} yr^{-1} in UHECR energy generation rate density, assuming iron-like nuclei."

    The interval is generated by varying the fraction of AICs that produce relativistic outflows and the acceleration efficiency inside broad uncertainty bands until the resulting energy generation rate overlaps the observed UHECR flux; the match is therefore obtained by construction once those parameters are treated as free.

full rationale

The paper models acceleration of heavy nuclei in relativistic outflows from AICs and concludes they can dominantly power observed UHECRs provided a majority of events host such outflows. The quoted energy generation rate density is obtained by folding in adjustable parameters for the outflow fraction, AIC rate, and acceleration efficiency; this produces a broad interval that can be tuned to encompass the observed UHECR flux. While the acceleration modeling itself may be independent, the load-bearing claim reduces to a consistency check once the adjustable fraction and efficiency are allowed to vary freely within 'uncertainties.' No self-citation chain or definitional loop is required for this reduction.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim depends on the prevalence of relativistic outflows in AIC events and on acceleration efficiencies that are not independently measured; these are treated as adjustable within broad uncertainties to reach the quoted energy density.

free parameters (2)
  • AIC event rate density
    Uncertain rate of accretion-induced collapses used to normalize the total energy output to observed UHECR levels.
  • acceleration efficiency for heavy nuclei
    Fraction of outflow energy converted into UHECRs; adjusted to produce the required flux.
axioms (1)
  • domain assumption A majority of AIC events produce magnetically dominated relativistic outflows with low entropy.
    Required for efficient heavy-nuclei formation and acceleration; stated as a conditional in the abstract.

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Reference graph

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