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arxiv: 2606.26495 · v1 · pith:CN7OZ7HCnew · submitted 2026-06-25 · 🌌 astro-ph.SR

Dust Formation in Common Envelope Binary Interactions -- III. Lightcurves

Chunliang Mu , Orsola De Marco , Luis C. Berm\'udez-Bustamante , Ryosuke Hirai , Daniel J. Price , Lionel Siess , Miguel Gonz\'alez-Bol\'ivar , Mike Y. M. Lau
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Nadejda Blagorodnova
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Pith reviewed 2026-06-26 04:29 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords common envelopeluminous red novaedust nucleationlight curvesbinary star interactionsasymptotic giant branchphotosphere expansion
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The pith

Simulations of common envelope binary interactions produce light curves with a hot peak, dust-induced decline, and cool plateau.

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

This paper performs post-processing light-curve calculations on two 3D hydrodynamic simulations of common envelope events between asymptotic giant branch stars and a compact companion, with dust nucleation included. The models run for 44 years under adiabatic conditions and show a bright hot peak lasting 3-5 years from photosphere expansion before and during inspiral. Dust forms 1-3 years after the interaction starts, triggering a sharp drop in bolometric luminosity, partial recovery, and a plateau at roughly 400 K effective temperature. The dust photosphere grows to about 250 au, with a prediction that it will turn optically thin at visible wavelengths in 100-200 years. The results are compared to specific observed luminous red novae while noting uncertainties from early surface resolution and the adiabatic assumption.

Core claim

Post-processing light-curve calculations for 3D simulations of common envelope binary interactions, including dust nucleation, reveal a bright hot peak lasting 3-5 years due to photospheric expansion before and during inspiral. Dust forms 1-3 years after the interaction begins, causing a sharp decline in bolometric luminosity followed by partial recovery and a plateau at an effective temperature of approximately 400 K. The dust photosphere grows to about 250 au, and is predicted to become optically thin at visible wavelengths between 100 and 200 years later, revealing an inner warmer photosphere.

What carries the argument

Post-processed light curves from 3D hydrodynamic simulations with dust nucleation

If this is right

  • Additional peaks appear at different times and for different viewing angles due to the asymmetry of the interaction.
  • The dust photosphere reaches a size of approximately 250 au by the end of the 44-year simulations.
  • Between 100 and 200 years after the interaction, the dust is expected to become optically thin at visible wavelengths, revealing an inner warmer photosphere.
  • The simulated light curves provide a match to observed events such as OGLE-2002-BLG-360 and AT 2025abao.

Where Pith is reading between the lines

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

  • The asymmetry of the common envelope interaction implies that observed light curves of luminous red novae depend strongly on the observer's viewing angle.
  • These results suggest that dust formation is a key process shaping the later evolution of common envelope transients.
  • Extending the simulations beyond adiabatic conditions could reveal how cooling affects the long-term light curve plateau.

Load-bearing premise

The hydrodynamic simulations assume adiabatic conditions over 44 years and have limited surface resolution in the initial phases.

What would settle it

An observed luminous red nova that shows no sharp luminosity decline 1-3 years after outburst onset or lacks a subsequent cool plateau at around 400 K would challenge the dust formation sequence in the models.

Figures

Figures reproduced from arXiv: 2606.26495 by Chunliang Mu, Daniel J. Price, Lionel Siess, Luis C. Berm\'udez-Bustamante, Miguel Gonz\'alez-Bol\'ivar, Mike Y. M. Lau, Nadejda Blagorodnova, Orsola De Marco, Ryosuke Hirai.

Figure 1
Figure 1. Figure 1: Opacity, 𝜅, optical depth, 𝜏, and temperature, 𝑇, along one line-of-sight as viewed from the polar 𝑧 → +∞ (blue) and the orbital 𝑦 → +∞ (orange) and 𝑥 → +∞ (green) directions, for the 1.7 M⊙ simulation at 𝑡 = 0 (top left), 𝑡 = 3 yr (top right), 𝑡 = 12 yr (bottom left), and 𝑡 = 20 yr (bottom right). The horizzontal dashed line in the middle panels marks 𝜏 = 2/3. The photospheric location is marked with blue… view at source ↗
Figure 2
Figure 2. Figure 2: Tabulatedmesa opacity, 𝜅MESA, as a function of temperature 𝑇 and density 𝜌. Grey cut-off line marks the approximate oxygen dust condensation temperature below which we override the opacity value with a constant gas opacity of 2 × 10−4 cm2g −1 . The table only covers regions with temperature above 631 K, although particles near the photosphere often have much lower temperatures. See text for details of how … view at source ↗
Figure 3
Figure 3. Figure 3: Dust (brown symbols to the left of 𝑇cutoff) and gas (cyan symbols to the right of 𝑇cutoff) opacities for all SPH particles as a function of their temperature for the 1.7 M⊙ dusty simulation at 𝑡 = 3 yr (top panel), 12 yr (middle panel), and 44 yr(bottom panel).When the SPH particle temperature is lower than 𝑇cutoff (green dashed vertical line), 𝜅gas = 2 × 10−4 cm2 g −1 , indicated by a blue dashed line. Th… view at source ↗
Figure 4
Figure 4. Figure 4: Surface brightness from each pixels for the 1.7 M⊙ (left two columns) and 3.7 M⊙ (right two columns) simulations, as viewed from the polar (𝑧 → +∞) direction (first and third columns) and the orbital (𝑦 → +∞) direction (second and fourth columns), at 𝑡 = 0, 3, 5.1, 12.1, and20.2 yr for the top, second, third, fourth and bottom rows, in each panel, respectively - note the progressively increasing size of th… view at source ↗
Figure 5
Figure 5. Figure 5: Bolometric luminosity lightcurve of the of the 1.7 M⊙ (left panels) and the 3.7 M⊙ (right panels) models for dusty (top panels) and non-dusty (bottom panels) simulations, integrated using a grid of 256 × 256 rays. Blue, orange, and green curves are the results viewed from +𝑧, +𝑦, and +𝑥 directions, respectively. The shaded areas are the calculated uncertainties (see Section 4.2). The light grey dashed line… view at source ↗
Figure 6
Figure 6. Figure 6: Spectral flux density as a function of wavelength for the 1.7 M⊙ (left column) and the 3.7 M⊙ (right column) dusty simulations, integrated using a grid of 256×256 rays, seen from 1 kpc. Blue, orange, and green are the three viewports, +𝑧, +𝑥 and +𝑦, respectively. The highest peak of 𝑓𝜆 (which is not the same as the peak of 𝜆 𝑓𝜆) is marked with a dashed vertical blue line. The colour reddens during the simu… view at source ↗
Figure 7
Figure 7. Figure 7: Evolution of the effective temperature, 𝑇eff, for the 1.7 M⊙ model (left panel) and the 3.7 M⊙ model (right panel). The thick lines indicate the temperature of the first, hot peak in the SED for two viewing directions. The presence of a corresponding thin line at a given moment in time indicates the presence of a second, cooler peak in the SED (evident in [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Photosphere radius as estimated by two distinct methods: a “geometric" method, using Equations 12 and 13 - solid lines, and an “observer’s" method - dot-dash and dashed lines for the 1.7 M⊙ (left panels) and 3.7 M⊙ (right panels) simulations, respectively. Blue (top panels) and orange (bottom panels) lines are for measurements in the 𝑧 → +∞ (polar) and 𝑦 → +∞ (orbital) directions, respectively. The dashed … view at source ↗
Figure 9
Figure 9. Figure 9: Grey optical depth of the dust shell, 𝜏d, for the 1.7 M⊙ (left panel) and the 3.7 M⊙ (right panel) simulations, observed from the three viewports. 𝜏d starts to drop after the first few decades, as expected by the free expansion model of the dust shell. Curves in the corresponding colours (dashed lines) use Equation 18 to fit data on the right of the grey vertical line and extrapolate the time when the dust… view at source ↗
Figure 10
Figure 10. Figure 10: Lightcurves of the 3.7 M⊙ dusty simulations as viewed from the polar (+𝑧) direction, comparing high resolution (1.3M particles, blue curve) and low resolution (200k particles, pink curve). The shaded areas are the error bars as computed following the method explained in Section 4.2 and Appendix F. ness of that pixel. In other words, we find the fraction of the highest contribution to the total effective p… view at source ↗
Figure 11
Figure 11. Figure 11: An estimate of the precision of the luminosity calculation, based on the number of particles, 𝑁res, used in the calculation of the specific intensity for each ray, for the 1.7 M⊙ simulation (the 3.7 M⊙ simulation is similar). Blue, orange, and green lines are averaged over a grid of 256 × 256 rays observed from the three three directions. SPH particle’s smoothing kernel, which, when the SPH particle is lo… view at source ↗
Figure 12
Figure 12. Figure 12: Absolute AB magnitude in Johnson V (solid), Cousins R (dotted), Cousins I (dash-dotted) and J bands (dashed) for the dusty 1.7 M⊙ (left panels) and 3.7 M⊙ (right panels) simulations, as viewed from polar (+𝑧, top panels) and equatorial (+𝑥, bottom panels) directions. The shaded area are uncertainties from lower surface resolution, the same as in [PITH_FULL_IMAGE:figures/full_fig_p013_12.png] view at source ↗
read the original abstract

Luminous red novae are transient events thought to arise from common envelope binary interactions. In this paper, we perform post-processing light-curve calculations for two, 3D hydrodynamic simulations of common envelope events. These simulations model interactions between 1.7 $M_\odot$ and 3.7 $M_\odot$ asymptotic giant branch stars and a 0.6 $M_\odot$ compact companion, including dust nucleation. In both our simulations, which are carried out for 44 years under adiabatic conditions, we observe a bright, hot peak lasting $3-5$ years, primarily due to the expansion of the photosphere before and during inspiral. Additional peaks can be seen appearing at different times and for different viewing angles, due to the asymmetry of the interaction. Dust forms about $1-3$ years after the beginning of the simulated interaction and shortly afterwards we witness a sharp decline in the bolometric luminosity, followed by a partial recovery and a plateau with an effective temperature of $\sim$400 K. The dust photosphere reaches a size of $\sim$250 au by the end of the simulations, but we predict that between 100 and 200 years, the dust will become optically thin at visible wavelengths, revealing an inner, warmer photosphere. The lightcurves obtained have two, well-quantified, but large uncertainties: insufficient surface resolution primarily affecting the first 1-2 years of the simulated lightcurves and the adiabatic assumption that affects primarily the later years. We finally contextualise our simulations within a group of observed luminous red nova transients, drawing particular attention to the outburst of OGLE-2002-BLG-360 and AT 2025abao, which are the closest match to our simulation.

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 performs post-processing light-curve calculations on two 44-year adiabatic 3D hydrodynamic simulations of common-envelope interactions (1.7 and 3.7 M⊙ AGB primaries with a 0.6 M⊙ companion, including dust nucleation). It reports a bright hot peak of 3–5 years driven by photospheric expansion before/during inspiral, dust formation at 1–3 years followed by a sharp bolometric decline, partial recovery, and a ~400 K plateau; the dust photosphere reaches ~250 au, with a prediction that it becomes optically thin at visible wavelengths between 100–200 years. Results are compared to observed luminous red novae, especially OGLE-2002-BLG-360 and AT 2025abao. The abstract explicitly flags two large uncertainties: insufficient surface resolution (primarily first 1–2 years) and the adiabatic assumption (primarily later years).

Significance. If the reported timelines and shapes prove robust, the work supplies the first multi-year, dust-inclusive light-curve predictions from 3D CE hydrodynamics and offers a concrete link between simulated photospheric expansion/dust nucleation and specific observed transients. The long integration time and inclusion of viewing-angle asymmetry are strengths.

major comments (2)
  1. [Abstract] Abstract: The central quantitative claims (3–5 yr bright hot peak, dust nucleation at 1–3 yr, subsequent sharp decline and ~400 K plateau, dust photosphere size ~250 au) are extracted from temperature and density fields whose evolution is controlled by the two explicitly flagged uncertainties whose time domains coincide exactly with the reported features. No resolution study or non-adiabatic run is described that would demonstrate that the quoted numbers survive changes in surface resolution or the inclusion of radiative losses.
  2. [Abstract] Abstract and § (light-curve post-processing description): Because the light curves are obtained by post-processing existing adiabatic hydro runs rather than by self-consistent radiation-hydrodynamics, any deviation from adiabaticity at late times directly alters the density–temperature trajectory that sets both the photospheric radius used for the early peak and the conditions for dust nucleation; the manuscript provides no independent check that the reported decline/plateau timing is insensitive to this assumption.
minor comments (2)
  1. [Abstract] The abstract states the two uncertainties are “well-quantified” but does not supply the actual quantification (e.g., convergence tests or estimated temperature errors); adding a short paragraph or table with those numbers would strengthen the presentation.
  2. Figure captions and text should explicitly label which viewing angles correspond to the additional peaks mentioned, to allow readers to assess the claimed asymmetry effects.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for acknowledging the potential significance of the first multi-year, dust-inclusive light-curve predictions from 3D common-envelope hydrodynamics. We address the two major comments below. Both comments correctly identify limitations that the manuscript already flags explicitly in the abstract; our responses explain why the reported results are still presented as baseline predictions from the available simulations.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central quantitative claims (3–5 yr bright hot peak, dust nucleation at 1–3 yr, subsequent sharp decline and ~400 K plateau, dust photosphere size ~250 au) are extracted from temperature and density fields whose evolution is controlled by the two explicitly flagged uncertainties whose time domains coincide exactly with the reported features. No resolution study or non-adiabatic run is described that would demonstrate that the quoted numbers survive changes in surface resolution or the inclusion of radiative losses.

    Authors: We agree that the reported timelines fall within the time domains affected by the two uncertainties already highlighted in the abstract. The quantitative values are therefore presented strictly as outcomes of the existing adiabatic simulations rather than as robust predictions independent of those assumptions. A dedicated resolution study or non-adiabatic hydrodynamic run lies outside the scope of this post-processing paper, which uses two previously published 44-year simulations. The manuscript therefore does not claim that the precise numbers (3–5 yr, 1–3 yr, ~250 au) would remain unchanged under different numerical or physical assumptions; instead it supplies the first concrete light-curve shapes and viewing-angle asymmetries obtainable from current 3D CE models that include dust nucleation. revision: no

  2. Referee: [Abstract] Abstract and § (light-curve post-processing description): Because the light curves are obtained by post-processing existing adiabatic hydro runs rather than by self-consistent radiation-hydrodynamics, any deviation from adiabaticity at late times directly alters the density–temperature trajectory that sets both the photospheric radius used for the early peak and the conditions for dust nucleation; the manuscript provides no independent check that the reported decline/plateau timing is insensitive to this assumption.

    Authors: We concur that the adiabatic assumption is a major limitation for the post-inspiral evolution and that the post-processing method cannot supply an independent verification of the decline/plateau timing. The early (3–5 yr) hot peak is driven by the dynamical photospheric expansion captured in the hydrodynamical runs before significant radiative losses are expected, while the later dust-related features are acknowledged to be sensitive to the adiabatic approximation. The paper therefore frames the ~400 K plateau and 100–200 yr optical thinning as illustrative outcomes under the stated assumptions, not as predictions guaranteed to survive the inclusion of radiative cooling. No additional check is possible without new radiation-hydrodynamic simulations. revision: no

Circularity Check

0 steps flagged

No significant circularity; results from post-processing of independent hydro simulations

full rationale

The paper computes lightcurves via post-processing of two pre-existing 3D adiabatic hydrodynamic simulations that already include dust nucleation. The reported timelines (3-5 yr hot peak, 1-3 yr dust formation, subsequent decline and ~400 K plateau) and sizes (~250 au dust photosphere) are direct numerical outputs from those simulations, not quantities defined by or fitted within the lightcurve post-processor itself. The manuscript flags resolution and adiabatic limitations but does not rename fitted parameters as predictions or reduce any central claim to a self-citation chain. No self-definitional, fitted-input, or ansatz-smuggling steps appear in the derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Abstract provides limited detail on model internals; main structural assumptions are the adiabatic evolution and dust nucleation treatment whose parameters are not enumerated here.

axioms (1)
  • domain assumption Adiabatic conditions throughout the 44-year hydrodynamic evolution
    Invoked for the full simulation duration and noted to affect later-year lightcurves.

pith-pipeline@v0.9.1-grok · 5904 in / 1360 out tokens · 30918 ms · 2026-06-26T04:29:21.656498+00:00 · methodology

discussion (0)

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