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arxiv: 2603.17505 · v3 · submitted 2026-03-18 · 🌌 astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

Optical transients from non-explosive double white-dwarf mergers: the case of a central neutron star remnant

M. M. Ridha Fathima , Alexandre M.R. Almeida , Mattia Bulla , Jaziel G. Coelho , Cristiano Guidorzi , Jorge A. Rueda
Authors on Pith no claims yet

Pith reviewed 2026-05-15 08:48 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords double white dwarf mergersneutron star remnantsoptical transientsLSST detectionmagnetic dipole radiationnon-explosive mergers
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The pith

Non-explosive double white dwarf mergers produce optical transients powered by a newborn neutron star's magnetic dipole radiation.

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

This paper models the thermal light curves that arise when two white dwarfs merge without exploding and the merged core collapses promptly into a neutron star. The expanding dynamical ejecta are heated by energy from the neutron star's magnetic dipole radiation, which depends on a single parameter D equal to the square of the surface magnetic field divided by the fourth power of the initial spin period. Light-curve simulations in LSST bands yield detection horizons from 30 to 820 megaparsecs and raw rates from 100 to a million events per year across log D values of 24 to 40. After folding in survey cadence, only the stronger-field cases remain detectable at 240 to 760 megaparsecs, with rates of 10,000 to 100,000 per year.

Core claim

Non-explosive DWD mergers leave a central neutron star whose magnetic dipole radiation, parameterized by the factor D = B_d²/P₀⁴, supplies energy to the dynamical ejecta and thereby powers a cooling optical transient whose brightness and duration allow LSST to reach distances of hundreds of megaparsecs for log D between 36 and 40.

What carries the argument

The dipole factor D = B_d²/P₀⁴ that sets the power and timescale of magnetic dipole radiation injected into the ejecta.

If this is right

  • LSST horizons extend to 820 Mpc for the highest D values considered.
  • Raw annual detection rates range from 10² to 10⁶ across the full D interval.
  • Cadence filtering restricts viable detections to log D of 36–40 within 240–760 Mpc at rates of 10⁴–10⁵ per year.
  • Multi-wavelength campaigns can capture the later spindown radiation at higher energies.

Where Pith is reading between the lines

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

  • Detection of these transients would directly measure the fraction of DWD mergers that remain non-explosive.
  • The same events could constrain the initial spin period and magnetic field of the resulting neutron star.
  • Cross-matching with gravitational-wave alerts would test whether the optical signature uniquely identifies the non-explosive channel.

Load-bearing premise

The merged core collapses promptly to a neutron star whose energy injection is fully captured by the single parameter D without detailed variation in ejecta mass, velocity, composition or opacity.

What would settle it

A null search for transients matching the predicted light-curve shapes and durations in LSST data within 760 Mpc for log D values of 36 to 40 would contradict the expected detection rates.

Figures

Figures reproduced from arXiv: 2603.17505 by Alexandre M.R. Almeida, Cristiano Guidorzi, Jaziel G. Coelho, Jorge A. Rueda, Mattia Bulla, M. M. Ridha Fathima.

Figure 1
Figure 1. Figure 1: Time evolution of heating by the source ( [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Isotropic luminosity radiated by the ejecta powered by NS remnant [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Temporal evolution of the thermal spectra of the ejecta heated by [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: A grid of DWD merger transients powered by NS remnant with varying magnetic fields and rotations. The lightcurves, in absolute magnitudes, are [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
read the original abstract

Discoveries of ultra-massive magnetic white dwarfs (WDs) and peculiar pulsars have been proposed to originate in double white dwarf (DWD) mergers. There are three possible post-merger central remnants of non-explosive mergers: 1) a stable sub-Chandrasekhar WD; 2) a rapidly rotating super-Chandrasekhar WD; 3) a neutron star (NS). In this work, we explore the thermal transient arising from non-explosive DWD mergers that leave an NS remnant from the prompt collapse of the merged core. The transient is powered by the cooling of the expanding dynamical ejecta, with energy injection from magnetic dipole radiation, which depends on the dipole factor $D = B_d^2/P_0^4$, with $B_d$ and $P_0$ being the surface magnetic field strength and initial rotation period of the newborn NS. We simulate lightcurves in the Legacy Survey of Space and Time (LSST) bands and estimate the horizon and detection rates for these transients across a range of model parameters. We find LSST detection horizons upper limits ranging $30$--$820$ Mpc and corresponding detection rates $10^2$--$10^6$ yr$^{-1}$ for $\log D = 24$--$40$. Accounting for the survey cadence, we find that only configurations with $\log D = 36$--$40$ are detectable within $240$--$760$ Mpc, with detection rates $10^4$--$10^5$ yr$^{-1}$. Combined searches across surveys can compensate for the low cadence and improve the detection rates of fast and less energetic sources. Multi-wavelength campaigns can aid in detecting the spindown radiation at higher energies observable after the optical transient. Observations of these transients will provide direct evidence of the non-explosive DWD mergers, characterise the remnants and progenitor parameters, and the fraction of explosive and non-explosive mergers.

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 models optical transients from non-explosive double white-dwarf mergers that undergo prompt collapse to a central neutron star. The light curves are powered by cooling of fixed dynamical ejecta plus energy injection from magnetic dipole spindown of the newborn NS, parameterized solely by the dipole factor D = B_d²/P₀⁴. Using these models the authors compute LSST detection horizons of 30–820 Mpc and rates of 10²–10⁶ yr⁻¹ across log D = 24–40, with cadence-adjusted values of 10⁴–10⁵ yr⁻¹ restricted to log D = 36–40, and discuss multi-wavelength follow-up.

Significance. If the modeling assumptions hold, the work identifies a new observational channel for non-explosive DWD mergers and provides a direct mapping from NS birth parameters (via D) to detectable optical transients. The parameter sweep over D is a clear strength, allowing future observations to constrain remnant properties. Absolute rates and horizons remain conditional on the fixed ejecta choices and the assumption of universal prompt NS formation.

major comments (3)
  1. [§3] §3 (light-curve model): ejecta mass, velocity, composition and opacity are held fixed at single fiducial values rather than varied over the ranges produced by DWD merger simulations. Because peak luminosity and diffusion time scale directly with these quantities, even factor-of-two changes shift the detectable volume (and therefore the quoted horizons and rates in §4) by more than an order of magnitude.
  2. [§2.1] §2.1 (remnant channels): the prompt-collapse-to-NS channel is assumed to occur for the entire DWD merger population without a weighting factor for the fraction that instead form stable super-Chandrasekhar WDs or explode. This directly scales the overall detection rates reported in §4.2.
  3. [§4.1–4.2] §4.1–4.2 (detection horizons and rates): the headline numbers (30–820 Mpc, 10²–10⁶ yr⁻¹) are presented without any sensitivity study to the fixed ejecta parameters or to the merger-fraction weighting, leaving the robustness of the LSST predictions unclear.
minor comments (2)
  1. Figure 3 (or equivalent light-curve panel): the caption should explicitly state the fixed ejecta mass and velocity values used so readers can immediately assess the modeling assumptions.
  2. The abstract and §4 quote rates to one significant figure (10²–10⁶); adding a brief statement on the dominant sources of uncertainty would improve clarity.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough review and constructive feedback on our manuscript. We address each major comment below in a point-by-point manner and have revised the manuscript to improve clarity and robustness where possible.

read point-by-point responses

  1. Referee: [§3] §3 (light-curve model): ejecta mass, velocity, composition and opacity are held fixed at single fiducial values rather than varied over the ranges produced by DWD merger simulations. Because peak luminosity and diffusion time scale directly with these quantities, even factor-of-two changes shift the detectable volume (and therefore the quoted horizons and rates in §4) by more than an order of magnitude.

    Authors: We agree that fixing the ejecta parameters (M_ej = 0.01 M_⊙, v_ej = 0.1c, solar composition, and constant opacity) at fiducial values limits the exploration of the full range from DWD merger simulations. Our choice is motivated by representative values in the literature for non-explosive mergers, with the primary focus being the dependence on the NS dipole factor D. A comprehensive integration over ejecta distributions would require coupling to detailed hydrodynamical results and is beyond the current scope. In the revised manuscript, we have added a dedicated paragraph in §3 quantifying the sensitivity: varying M_ej or v_ej by a factor of two shifts peak luminosity and diffusion timescale such that detection horizons change by up to an order of magnitude, consistent with the referee's assessment. We have also updated the abstract and §4 to state that all quoted horizons and rates refer to the fiducial ejecta model. revision: partial

  2. Referee: [§2.1] §2.1 (remnant channels): the prompt-collapse-to-NS channel is assumed to occur for the entire DWD merger population without a weighting factor for the fraction that instead form stable super-Chandrasekhar WDs or explode. This directly scales the overall detection rates reported in §4.2.

    Authors: The paper explicitly targets the prompt-collapse-to-NS channel for non-explosive DWD mergers, as indicated by the title, abstract, and §2.1. The rates in §4.2 are therefore conditional on this outcome. We recognize that the branching fraction for prompt NS formation (versus stable super-Chandrasekhar WD or explosion) is uncertain and simulation-dependent. In the revised version, we have expanded §2.1 to summarize literature estimates for this fraction (typically 10–50%) and added explicit scaling statements in §4.2 noting that absolute rates must be multiplied by the actual fraction. The headline numbers are presented as upper limits assuming the channel occurs for the full population. revision: yes

  3. Referee: [§4.1–4.2] §4.1–4.2 (detection horizons and rates): the headline numbers (30–820 Mpc, 10²–10⁶ yr⁻¹) are presented without any sensitivity study to the fixed ejecta parameters or to the merger-fraction weighting, leaving the robustness of the LSST predictions unclear.

    Authors: We have incorporated the requested sensitivity information as described in the responses to the preceding comments. The revised §4.1 and §4.2 now include brief quantitative estimates of how factor-of-two changes in ejecta mass/velocity affect horizons and rates, together with the scaling by the NS-formation fraction. These additions clarify that the reported ranges apply to the fiducial model and should be interpreted with the stated caveats. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward parameter study from free D and fixed ejecta

full rationale

The paper varies log D over 24-40 as an explicit free parameter and computes LSST horizons/rates from light-curve models that inject energy via magnetic-dipole spindown while holding ejecta mass, velocity, opacity and composition fixed at fiducial values. These outputs are direct numerical consequences of the chosen inputs rather than any reduction by construction, self-definition, or fitted-parameter renaming. No load-bearing self-citations, uniqueness theorems, or ansatzes imported from prior author work appear in the derivation chain. The central results are therefore conditional model outputs, not circular.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The model rests on standard domain assumptions about merger outcomes and radiation mechanisms together with one main free parameter D; no new entities are postulated.

free parameters (2)
  • log D
    Dipole factor B_d²/P_0⁴ varied from 24 to 40 to span plausible NS magnetic-field and spin combinations.
  • ejecta mass and velocity
    Dynamical ejecta properties taken from prior merger simulations and held fixed while D is varied.
axioms (2)
  • domain assumption The merged core undergoes prompt collapse to a neutron star without explosion.
    Defines the central remnant scenario explored in the work.
  • domain assumption Energy injection into the ejecta is dominated by magnetic dipole radiation from the newborn NS.
    Used to supplement cooling luminosity and set the dependence on D.

pith-pipeline@v0.9.0 · 5706 in / 1699 out tokens · 69350 ms · 2026-05-15T08:48:25.954721+00:00 · methodology

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