pith. sign in

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
show 1 more author
Nadejda Blagorodnova
This is my paper

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
0
0 comments X

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)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

300 extracted references · 251 canonical work pages · 14 internal anchors

  1. [1]

    SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations

    splash: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations. , keywords =. doi:10.1071/AS07022 , archivePrefix =. 0709.0832 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1071/as07022

  2. [2]

    , keywords =

    Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes. , keywords =. doi:10.3847/2041-8213/ad6862 , archivePrefix =. 2404.09381 , primaryClass =

    work page doi:10.3847/2041-8213/ad6862 2041

  3. [3]

    Forbidden hugs in pandemic times. IV. Panchromatic evolution of three luminous red novae. , keywords =. doi:10.1051/0004-6361/202244684 , archivePrefix =. 2208.02782 , primaryClass =

    work page doi:10.1051/0004-6361/202244684

  4. [4]

    SN 1997bs in M66: Another Extragalactic Eta Carinae Analog?

    SN 1997bs in M66: Another Extragalactic Eta Carinae Analog?. , keywords =. doi:10.1086/317727 , archivePrefix =. astro-ph/0009027 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/317727

  5. [5]

    , keywords =

    The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor. , keywords =. doi:10.1051/0004-6361/202140525 , archivePrefix =. 2102.05662 , primaryClass =

    work page doi:10.1051/0004-6361/202140525

  6. [6]

    Forbidden hugs in pandemic times. III. Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631. , keywords =. doi:10.1051/0004-6361/202244393 , archivePrefix =. 2207.00734 , primaryClass =

    work page doi:10.1051/0004-6361/202244393

  7. [7]

    Stellar models

    Simulating a stellar contact binary merger - I. Stellar models. , keywords =. doi:10.1093/mnras/stab2140 , archivePrefix =. 2107.11480 , primaryClass =

    work page doi:10.1093/mnras/stab2140

  8. [8]

    doi:10.5281/zenodo.14712174 , version =

    Fouesneau, Morgan , title =. doi:10.5281/zenodo.14712174 , url =

    work page doi:10.5281/zenodo.14712174

  9. [9]

    2002, Earth Moon and Planets, 90, 1,

    UBVRI passbands. , keywords =. doi:10.1086/132749 , adsurl =

    work page doi:10.1086/132749

  10. [10]

    , keywords =

    From 3D hydrodynamic simulations of common-envelope interaction to gravitational-wave mergers. , keywords =. doi:10.1051/0004-6361/202142731 , archivePrefix =. 2111.12112 , primaryClass =

    work page doi:10.1051/0004-6361/202142731

  11. [11]

    Simulating a Stellar Binary Merger. II. Obtaining a Light Curve. , keywords =. doi:10.3847/1538-4357/ada6b8 , archivePrefix =. 2412.06583 , primaryClass =

    work page doi:10.3847/1538-4357/ada6b8

  12. [12]

    3D simulations of AGB stellar winds. II. Ray-tracer implementation and impact of radiation on the outflow morphology. , keywords =. doi:10.1051/0004-6361/202346282 , archivePrefix =. 2304.09786 , primaryClass =

    work page doi:10.1051/0004-6361/202346282

  13. [13]

    The obstructive role of radiation transport in envelope ejection

    Common envelopes in massive stars: III. The obstructive role of radiation transport in envelope ejection. , keywords =. doi:10.1051/0004-6361/202554782 , archivePrefix =. 2503.20506 , primaryClass =

    work page doi:10.1051/0004-6361/202554782

  14. [14]

    Shock-powered light curves of luminous red novae as signatures of pre-dynamical mass loss in stellar mergers

    Shock-powered light curves of luminous red novae as signatures of pre-dynamical mass-loss in stellar mergers. , keywords =. doi:10.1093/mnras/stx1768 , archivePrefix =. 1705.03895 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1768

  15. [15]

    , keywords =

    Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force. , keywords =. doi:10.3847/2041-8213/ad2a47 , archivePrefix =. 2402.05686 , primaryClass =

    work page doi:10.3847/2041-8213/ad2a47 2041

  16. [16]

    , keywords =

    Hot Springs and Dust Reservoirs: JWST Reveals the Dusty, Molecular Aftermath of Extragalactic Stellar Mergers. , keywords =. doi:10.3847/1538-4357/ae38bf , archivePrefix =. 2508.03932 , primaryClass =

    work page doi:10.3847/1538-4357/ae38bf

  17. [17]

    Lessons from the Onset of a Common Envelope Episode: the Remarkable M31 2015 Luminous Red Nova Outburst

    Lessons from the Onset of a Common Envelope Episode: the Remarkable M31 2015 Luminous Red Nova Outburst. , keywords =. doi:10.3847/1538-4357/835/2/282 , archivePrefix =. 1605.01493 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/835/2/282 2015

  18. [18]

    , keywords =

    Luminous red novae: Stellar mergers or giant eruptions?. , keywords =. doi:10.1051/0004-6361/201935999 , archivePrefix =. 1906.00812 , primaryClass =

    work page doi:10.1051/0004-6361/201935999 1906

  19. [19]

    Living Reviews in Computational Astrophysics , keywords =

    Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques. Living Reviews in Computational Astrophysics , keywords =. doi:10.1007/s41115-023-00017-x , archivePrefix =. 2212.07308 , primaryClass =

    work page doi:10.1007/s41115-023-00017-x

  20. [20]

    , keywords =

    Dust formation in common envelope binary interaction - I: 3D simulations using the Bowen approximation. , keywords =. doi:10.1093/mnras/stad3748 , archivePrefix =. 2306.16609 , primaryClass =

    work page doi:10.1093/mnras/stad3748

  21. [21]

    Low Temperature Opacities

    Low-Temperature Opacities. , keywords =. doi:10.1086/428642 , archivePrefix =. astro-ph/0502045 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/428642

  22. [22]

    Tricco , title =

    Andrew Harris and Terrence S. Tricco , title =. 2023 , publisher =. doi:10.21105/joss.05263 , url =

    work page doi:10.21105/joss.05263 2023

  23. [23]

    The Limiting Effects of Dust in Brown Dwarf Model Atmospheres

    The Limiting Effects of Dust in Brown Dwarf Model Atmospheres. , keywords =. doi:10.1086/321547 , archivePrefix =. astro-ph/0104256 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/321547

  24. [24]

    , keywords =

    3D models of the circumstellar environments of evolved stars: Formation of multiple spiral structures. , keywords =. doi:10.1093/mnras/stac749 , archivePrefix =. 2203.08318 , primaryClass =

    work page doi:10.1093/mnras/stac749

  25. [25]

    , keywords =

    A 3D Radiation Hydrodynamic AGB Binary Model. , keywords =. doi:10.3847/1538-4357/ab7b6e , archivePrefix =. 1910.08027 , primaryClass =

    work page doi:10.3847/1538-4357/ab7b6e 1910

  26. [26]

    Mass Transfer and Disc Formation in AGB Binary Systems

    Mass transfer and disc formation in AGB binary systems. , keywords =. doi:10.1093/mnras/stx680 , archivePrefix =. 1702.06160 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx680

  27. [27]

    The central stars of NGC 2346, He 2-36 and NGC 3132

    A-type central stars of planetary nebulae - II. The central stars of NGC 2346, He 2-36 and NGC 3132. , year = 1978, month = dec, volume = 185, pages =

    1978

  28. [28]

    doi:10.1093/mnras/stv701 , Eprint =

    Likely detection of water-rich asteroid debris in a metal-polluted white dwarf. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stv701 , adsurl =

    work page doi:10.1093/mnras/stv701

  29. [29]

    , archivePrefix = "arXiv", eprint =

    The frequency and infrared brightness of circumstellar discs at white dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stv282 , adsurl =

    work page doi:10.1093/mnras/stv282

  30. [30]

    , archivePrefix = "arXiv", eprint =

    Detectable close-in planets around white dwarfs through late unpacking. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu2475 , adsurl =

    work page doi:10.1093/mnras/stu2475

  31. [31]

    , archivePrefix = "arXiv", eprint =

    Evidence for an Anhydrous Carbonaceous Extrasolar Minor Planet. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/799/1/109 , adsurl =

    work page doi:10.1088/0004-637x/799/1/109

  32. [32]

    , archivePrefix = "arXiv", eprint =

    Hydrogen delivery onto white dwarfs from remnant exo-Oort cloud comets. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu2026 , adsurl =

    work page doi:10.1093/mnras/stu2026

  33. [33]

    Tidal disruption of an extremely eccentric asteroid

    Formation of planetary debris discs around white dwarfs - I. Tidal disruption of an extremely eccentric asteroid. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu1871 , adsurl =

    work page doi:10.1093/mnras/stu1871

  34. [34]

    , archivePrefix = "arXiv", eprint =

    Variable emission from a gaseous disc around a metal-polluted white dwarf. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu1876 , adsurl =

    work page doi:10.1093/mnras/stu1876

  35. [35]

    , archivePrefix = "arXiv", eprint =

    Comparison of Atmospheric Parameters Determined from Spectroscopy and Photometry for DA White Dwarfs in the Sloan Digital Sky Survey. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/796/2/128 , adsurl =

    work page doi:10.1088/0004-637x/796/2/128

  36. [36]

    , archivePrefix = "arXiv", eprint =

    Non-LTE spectral models for the gaseous debris-disk component of Ton 345. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201423690 , adsurl =

    work page doi:10.1051/0004-6361/201423690

  37. [37]

    , archivePrefix = "arXiv", eprint =

    The Drop during Less than 300 Days of a Dusty White Dwarf's Infrared Luminosity. , archivePrefix = "arXiv", eprint =. doi:10.1088/2041-8205/792/2/L39 , adsurl =

    work page doi:10.1088/2041-8205/792/2/l39 2041

  38. [38]

    , archivePrefix = "arXiv", eprint =

    Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201118391 , adsurl =

    work page doi:10.1051/0004-6361/201118391

  39. [39]

    , archivePrefix = "arXiv", eprint =

    The frequency of planetary debris around young white dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201423691 , adsurl =

    work page doi:10.1051/0004-6361/201423691

  40. [40]

    , archivePrefix = "arXiv", eprint =

    Evidence for an external origin of heavy elements in hot DA white dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu216 , adsurl =

    work page doi:10.1093/mnras/stu216

  41. [41]

    Annual Review of Earth and Planetary Sciences , year = 2014, month = may, volume = 42, pages =

    Extrasolar Cosmochemistry. Annual Review of Earth and Planetary Sciences , year = 2014, month = may, volume = 42, pages =. doi:10.1146/annurev-earth-060313-054740 , adsurl =

    work page doi:10.1146/annurev-earth-060313-054740 2014

  42. [42]

    , archivePrefix = "arXiv", eprint =

    Dusty WDs in the WISE All Sky Survey SDSS. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/786/2/77 , adsurl =

    work page doi:10.1088/0004-637x/786/2/77

  43. [43]

    The X-shooter Spectral Library (XSL). I. DR1: Near-ultraviolet through optical spectra from the first year of the survey. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201322505 , adsurl =

    work page doi:10.1051/0004-6361/201322505

  44. [44]

    , archivePrefix = "arXiv", eprint =

    Elemental Compositions of Two Extrasolar Rocky Planetesimals. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/783/2/79 , adsurl =

    work page doi:10.1088/0004-637x/783/2/79

  45. [45]

    , archivePrefix = "arXiv", eprint =

    Radiative levitation of silicon in the atmospheres of two Hyades DA white dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnrasl/slt149 , adsurl =

    work page doi:10.1093/mnrasl/slt149

  46. [46]

    Science , archivePrefix = "arXiv", eprint =

    Evidence for Water in the Rocky Debris of a Disrupted Extrasolar Minor Planet. Science , archivePrefix = "arXiv", eprint =. doi:10.1126/science.1239447 , adsurl =

    work page doi:10.1126/science.1239447

  47. [47]

    , archivePrefix = "arXiv", eprint =

    Two Beyond-primitive Extrasolar Planetesimals. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/766/2/132 , adsurl =

    work page doi:10.1088/0004-637x/766/2/132

  48. [48]

    Proceedings of the National Academy of Science , year = 2012, month = nov, volume = 109, pages =

    Carbon and other light element contents in the Earth's core based on first-principles molecular dynamics. Proceedings of the National Academy of Science , year = 2012, month = nov, volume = 109, pages =. doi:10.1073/pnas.1203826109 , adsurl =

    work page doi:10.1073/pnas.1203826109 2012

  49. [49]

    E., & Jackson, A

    The chemical diversity of exo-terrestrial planetary debris around white dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2012.21201.x , adsurl =

    work page doi:10.1111/j.1365-2966.2012.21201.x 2012

  50. [50]

    , archivePrefix = "arXiv", eprint =

    Gaseous Material Orbiting the Polluted, Dusty White Dwarf HE 1349-2305. , archivePrefix = "arXiv", eprint =. doi:10.1088/2041-8205/751/1/L4 , adsurl =

    work page doi:10.1088/2041-8205/751/1/l4 2041

  51. [51]

    Double core evolution. I. A 16 M sun star with a 1 M sun neutron-star companion. , keywords =. 1978. doi:10.1086/156142 , adsurl =

    work page doi:10.1086/156142 1978

  52. [52]

    , archivePrefix = "arXiv", eprint =

    Detection of Keplerian dynamics in a disk around the post-AGB star AC Herculis. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201525742 , adsurl =

    work page doi:10.1051/0004-6361/201525742

  53. [53]

    The effect of a wider initial separation on common envelope binary interaction simulations

    The effect of a wider initial separation on common envelope binary interaction simulations. , keywords =. doi:10.1093/mnras/stw2377 , archivePrefix =. 1603.01953 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2377

  54. [54]

    , keywords =

    Formation pathway for lonely stripped-envelope supernova progenitors: implications for Cassiopeia A. , keywords =. doi:10.1093/mnras/staa2898 , archivePrefix =. 2008.05076 , primaryClass =

    work page doi:10.1093/mnras/staa2898 2008

  55. [55]

    J., & Ogilvie, G

    E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh. , keywords =. doi:10.1111/j.1365-2966.2009.15715.x , archivePrefix =. 0901.4107 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15715.x 2009

  56. [56]

    Journal of Computational Physics , year = 2013, month = mar, volume =

    Efficient parallelization for AMR MHD multiphysics calculations; implementation in AstroBEAR. Journal of Computational Physics , year = 2013, month = mar, volume =. doi:10.1016/j.jcp.2012.10.004 , adsurl =

    work page doi:10.1016/j.jcp.2012.10.004 2013

  57. [57]

    , keywords =

    Properties of the post in-spiral common envelope ejecta II: dust formation. , keywords =. doi:10.1093/mnras/staa2169 , archivePrefix =. 2003.06151 , primaryClass =

    work page doi:10.1093/mnras/staa2169 2003

  58. [58]

    Dynamical and thermal evolution

    Properties of the post-inspiral common envelope ejecta - I. Dynamical and thermal evolution. , keywords =. 2019. doi:10.1093/mnras/stz2312 , archivePrefix =. 1907.03980 , primaryClass =

    work page doi:10.1093/mnras/stz2312 2019

  59. [59]

    , keywords =

    Density Conversion between 1D and 3D Stellar Models with ^ 1D MESA2HYDRO ^ 3D. , keywords =. 2019. doi:10.3847/1538-4357/ab3405 , archivePrefix =. 1907.09062 , primaryClass =

    work page doi:10.3847/1538-4357/ab3405 2019

  60. [60]

    , keywords =

    Speaking with one voice: simulations and observations discuss the common envelope parameter. , keywords =. 2019. doi:10.1093/mnras/stz2756 , archivePrefix =. 1902.02039 , primaryClass =

    work page doi:10.1093/mnras/stz2756 2019

  61. [61]

    Extending Common Envelope Simulations from Roche Lobe Overflow to the Nebular Phase

    Extending common envelope simulations from Roche lobe overflow to the nebular phase. , keywords =. doi:10.1093/mnras/sty3485 , archivePrefix =. 1809.02297 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty3485

  62. [62]

    Monthly Notices of the Royal Astronomical Society , volume=

    The impact of recombination energy on simulations of the common-envelope binary interaction , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2020 , publisher=

    2020

  63. [63]

    Smoothed Particle Hydrodynamics and Magnetohydrodynamics

    Smoothed particle hydrodynamics and magnetohydrodynamics. Journal of Computational Physics , keywords =. doi:10.1016/j.jcp.2010.12.011 , archivePrefix =. 1012.1885 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.jcp.2010.12.011 2010

  64. [64]

    Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics

    Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics. , keywords =. 2018. doi:10.1017/pasa.2018.25 , archivePrefix =. 1702.03930 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pasa.2018.25 2018

  65. [65]

    J., & Ogilvie, G

    Super asymptotic giant branch stars. I - Evolution code comparison. , keywords =. 2010. doi:10.1111/j.1365-2966.2009.15772.x , adsurl =

    work page doi:10.1111/j.1365-2966.2009.15772.x 2010

  66. [66]

    Evolution of massive AGB stars. III. the thermally pulsing super-AGB phase. , keywords =. 2010. doi:10.1051/0004-6361/200913556 , adsurl =

    work page doi:10.1051/0004-6361/200913556 2010

  67. [67]

    , archivePrefix = "arXiv", eprint =

    A mid-IR interferometric survey with MIDI/VLTI: resolving the second-generation protoplanetary disks around post-AGB binaries. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201629161 , adsurl =

    work page doi:10.1051/0004-6361/201629161

  68. [68]

    arXiv e-prints , archivePrefix = "arXiv", eprint =

    Gas Flows Within Cavities of Circumbinary Discs in Eccentric Binary Protostellar Systems. arXiv e-prints , archivePrefix = "arXiv", eprint =

  69. [69]

    , archivePrefix = "arXiv", eprint =

    The planets around NN Serpentis: still there. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stt1903 , adsurl =

    work page doi:10.1093/mnras/stt1903

  70. [70]

    , archivePrefix = "arXiv", eprint =

    A Spitzer Space Telescope Study of the Debris Disks around Four SDSS White Dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/750/1/86 , adsurl =

    work page doi:10.1088/0004-637x/750/1/86

  71. [71]

    , archivePrefix = "arXiv", eprint =

    Two Extrasolar Asteroids with Low Volatile-element Mass Fractions. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/750/1/69 , adsurl =

    work page doi:10.1088/0004-637x/750/1/69

  72. [72]

    E., & Jackson, A

    A trio of metal-rich dust and gas discs found orbiting candidate white dwarfs with K-band excess. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2012.20421.x , adsurl =

    work page doi:10.1111/j.1365-2966.2012.20421.x 2012

  73. [73]

    , archivePrefix = "arXiv", eprint =

    Constraints on the Lifetimes of Disks Resulting from Tidally Destroyed Rocky Planetary Bodies. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/749/2/154 , adsurl =

    work page doi:10.1088/0004-637x/749/2/154

  74. [74]

    , archivePrefix = "arXiv", eprint =

    Detailed Compositional Analysis of the Heavily Polluted DBZ White Dwarf SDSS J073842.56+183509.06: A Window on Planet Formation?. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/749/1/6 , adsurl =

    work page doi:10.1088/0004-637x/749/1/6

  75. [75]

    , archivePrefix = "arXiv", eprint =

    The Link between Planetary Systems, Dusty White Dwarfs, and Metal-polluted White Dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/747/2/148 , adsurl =

    work page doi:10.1088/0004-637x/747/2/148

  76. [76]

    , archivePrefix = "arXiv", eprint =

    The Cosmic Origins Spectrograph. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/744/1/60 , adsurl =

    work page doi:10.1088/0004-637x/744/1/60

  77. [77]

    , archivePrefix = "arXiv", eprint =

    Water Fractions in Extrasolar Planetesimals. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-6256/143/1/6 , adsurl =

    work page doi:10.1088/0004-6256/143/1/6

  78. [78]

    , archivePrefix = "arXiv", eprint =

    X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201117752 , adsurl =

    work page doi:10.1051/0004-6361/201117752

  79. [79]

    , archivePrefix = "arXiv", eprint =

    Rocky Extrasolar Planetary Compositions Derived from Externally Polluted White Dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/741/1/64 , adsurl =

    work page doi:10.1088/0004-637x/741/1/64

  80. [80]

    Monthly Notices of the Royal Astronomical Society , author =

    DA white dwarfs in Sloan Digital Sky Survey Data Release 7 and a search for infrared excess emission. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2011.19337.x , adsurl =

    work page doi:10.1111/j.1365-2966.2011.19337.x 2011

Showing first 80 references.