Modelling depletion by re-accretion of gas from a dusty disc in post-AGB stars

Gijs Nelemans; Glenn-Michael Oomen; Hans Van Winckel; Onno Pols

REVIEW 3 major objections 4 minor 1 cited by

Modelling depletion by re-accretion of gas from a dusty disc in post-AGB stars

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read Re-accretion of metal-poor gas from a circumbinary disc can reproduce the observed depletion of post-AGB stars, provided the disc begins with a mass near $10^{-2}\,M_\odot$ and initial accretion rates of at least about…

desk verdict Solid, useful MESA study of depletion by re-accretion, but the headline accretion-rate constraint is a factor of ~6 too strong once the uncalibrated wind law is varied, so the abstract oversells the lower bound. read the letter →

arxiv 1908.01788 v2 pith:Q75JBCYP submitted 2019-08-05 astro-ph.SR

Glenn-Michael Oomen , Hans Van Winckel , Onno Pols , Gijs Nelemans This is my paper · ORCID

classification astro-ph.SR

keywords post-AGBstarscircumbinarydiscschemicaldepletionrefractoryelementabundancesgasaccretionpost-RGBstellarevolutionmodelsabundancepatterns

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Many binary post-AGB stars show photospheric underabundances of elements that condense into dust at high temperatures, a pattern called depletion. The paper argues that this happens because metal-poor gas re-accretes from a circumbinary disc while dust is pushed away, and it tests the idea with stellar-evolution models that add such gas to stars and compare them with 58 observed disc-type post-AGB stars. To match the observed depletion, especially in cool stars, the models require initial accretion rates of at least about $3\times10^{-7}\,M_\odot\,\mathrm{yr}^{-1}$ and initial disc masses near $10^{-2}\,M_\odot$. At these rates accretion also lengthens post-AGB evolution by a factor of two to five, and the models reproduce the observed mix of saturated and plateau-shaped depletion patterns, with plateau patterns expected mainly among slowly evolving post-RGB stars.

What carries the argument

The load-bearing mechanism is gas dilution of the outer convective envelope by a time-dependent accretion flow. The disc drains viscously with rate $\dot{M}(t)=\dot{M}(0)(1+4\dot{M}(0)t/M_d)^{-3/2}$, where $\dot{M}(0)$ is the initial accretion rate and $M_d$ the initial disc mass; half the inflowing gas goes to the post-AGB star and half to the companion. The accreted gas has refractory-element abundances suppressed by up to $-4$ dex relative to the star's initial composition (calibrated from the most depleted observed objects), and as it mixes into the shrinking convective envelope it drives down photospheric $[\mathrm{Zn/Ti}]$ at a rate set by the ratio of the depletion timescale to the evolutionary timescale. The comparison is made in the $T_\mathrm{eff}$ versus $[\mathrm{Zn/Ti}]$ plane, where an observed star must lie on or below a model curve if some choice of accreted composition is to explain it.

What would settle it

A decisive test would be to measure the disc mass of a strongly depleted star with $T_\mathrm{eff}\lesssim5000$ K and luminosity above $7500\,L_\odot$: the model requires $\dot{M}(0)\gtrsim3\times10^{-7}\,M_\odot\,\mathrm{yr}^{-1}$ and $M_d\sim10^{-2}\,M_\odot$ for such an object, so a disc found below $10^{-3}\,M_\odot$ would falsify the required parameter range. A second check is to compare turn-off temperatures of depletion patterns with independently measured orbital separations; the model's single accreted composition predicts they should not vary, while observed variation would show the input-composition assumption is wrong.

Watch

Extended reading notes

Core claim

The paper's central claim is that the chemical peculiarity called depletion in disc-type post-AGB stars is produced by re-accretion of metal-poor gas from a circumbinary disc, and that this mechanism works without fine tuning only when the disc starts massive and feeds the binary fast. Using models that add a refractory-element-poor gas to evolving post-AGB envelopes and comparing them with 58 observed stars, the paper finds that initial accretion rates below about $5\times10^{-8}\,M_\odot\,\mathrm{yr}^{-1}$ rarely produce depleted photospheres before the star becomes hot, while initial rates of $\gtrsim3\times10^{-7}\,M_\odot\,\mathrm{yr}^{-1}$ together with disc masses near $10^{-2}\,M_\odot$ reproduce the observed depleted stars, including cool, mildly depleted post-RGB objects. The same accretion delays the stellar evolution track, extending the post-AGB phase by a factor of two to five. The paper also argues that the diversity of depletion patterns follows from how far dilution has proceeded: plateau patterns are partially diluted envelopes, saturated patterns have converged to the composition of the accreted gas, and the turn-off temperature itself reflects the composition of the gas supplied by the disc.

Load-bearing premise

The models assume one universal chemical composition for the accreted gas, fixed by the most depleted stars in the sample; if the real accreted gas is less metal-poor or differs from star to star, the predicted depletion curves, minimum accretion rates, and required disc masses all shift.

Editorial extensions

If this is right

Observed depletion becomes a signpost of a massive infant disc: stars that are depleted at low effective temperature must have started with $M_d\sim10^{-2}\,M_\odot$ and $\dot{M}(0)\gtrsim3\times10^{-7}\,M_\odot\,\mathrm{yr}^{-1}$.
Post-AGB lifetimes are not set by nuclear burning and winds alone; accretion can stretch them by a factor of two for low-mass post-RGB stars and up to five for more massive post-AGB stars, so planetary-nebula formation and dispersal calculations should include this effect.
Saturated abundance patterns should be common because massive post-AGB stars dilute their envelopes quickly; plateau patterns should be rarer and preferentially found in the slower-evolving post-RGB systems.
Post-RGB stars can become depleted below about 5000 K, while $0.65\,M_\odot$ post-AGB stars only deplete above roughly 6000 K, cleanly separating the two populations in the $T_\mathrm{eff}$ versus $[\mathrm{Zn/Ti}]$ plane.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If the required disc masses are correct, then non-depleted disc stars are probably not missing the accretion mechanism but started with smaller discs or began accreting later; the paper's own dilution logic implies their accreted gas may also be less depleted.
A testable consequence the paper leaves implicit is that the observed spread in turn-off temperatures (800 to 1500 K) should correlate with orbital separation, because the inner gas-disc radius is set by binary properties while dust sublimation is set by stellar luminosity; interferometric disc radii could check this.
Because accretion extends post-AGB lifetimes by factors of two to five, counts of post-AGB stars and planetary nebulae may imply lower birth rates than previously estimated, and population synthesis using these lifetimes would revise inferred binary-interaction rates.
A direct extension would apply the same accretion prescription to post-RGB binaries with measured orbital periods, since the paper predicts lower accretion rates suffice there; a sample with pulsation-based luminosities could test the luminosity-bin classification.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Colleague,

Here's my read of Oomen et al. The qualitative mechanism is probably right; the quantitative headline is not as firm as the abstract suggests.

The genuinely new piece is the first set of MESA post-AGB/post-RGB models that include time-dependent accretion from a viscously evolving circumbinary disc, with a nuclear network extended to cover the refractory elements that trace depletion. The parameter study is thorough: five core masses, five initial accretion rates, three disc masses, four accretion start temperatures, plus explicit sensitivity runs for mixing depth and wind strength. Comparing the models to a 58-star observed sample with Gaia-based luminosities is a real step forward. The result that accretion can stretch post-AGB evolution timescales by factors of 2-5 is interesting and likely robust in direction.

The soft spots are in the quantitative claims. The abstract states that initial accretion rates >=3e-7 Msun/yr and disc masses ~1e-2 Msun are needed. But the wind law used for cool post-AGB stars (Schroder & Cuntz) is not calibrated for these objects; the authors themselves note that it is a chromospheric-activity wind and that Cranmer & Saar find it unsuitable. Their own Fig. 16 shows that a 10x weaker wind lets a 5e-8 Msun/yr model become depleted at 5000-6000 K. That is a factor of 6 below the headline threshold. Since the boundary between depleted and non-depleted stars at low Teff is what constrains the accretion rate, the lower bound is conditional on an unknown wind law. The authors flag this in the discussion, but the abstract and conclusions do not carry the caveat.

Second, the composition of the accreted gas is calibrated from the most depleted observed stars (Sect. 3.2, Fig. 2). The models then reproduce the saturated abundance patterns by construction. They do acknowledge the diversity in turn-off temperatures and that one composition cannot fit all stars, and they present the models as upper limits on depletion. Still, the phrase 'successfully accounts for the chemical peculiarity' overstates the independence of the check.

Minor issues: no hash or direct link to the MESA inlists (only a promise), and the model-observation comparisons are visual, without propagated errors. These are easy to fix.

Overall, this is a serious piece of work for the post-AGB/binary/PN community. It deserves peer review. The authors should be asked to either calibrate the cool wind or explicitly present the accretion-rate constraints as functions of wind strength, and to soften the abstract accordingly. The circularity in the gas composition should be made more prominent. With those revisions, the paper would be a solid contribution.

Referee Report

3 major / 4 minor

Summary. The paper models the post-AGB and post-RGB evolution of stars that accrete refractory-depleted gas from a circumbinary disc, using MESA tracks for core masses 0.40-0.65 Msun and a viscous disc model for the time-dependent accretion rate. The accreted-gas abundance pattern is calibrated from the most depleted observed post-AGB stars, and the model tracks are compared in the Teff-[Zn/Ti] plane with a sample of 58 Galactic disc-type post-AGB stars whose luminosities are estimated from Gaia DR2 distances. The main claims are that high initial accretion rates (≳3e-7 Msun/yr) and large initial disc masses (~1e-2 Msun) are needed to reproduce depleted post-AGB stars, that accretion can extend the post-AGB evolution timescale by factors of 2-5, that unsaturated plateau patterns should be more common among post-RGB stars, and that post-RGB stars can become depleted at lower effective temperatures than post-AGB stars.

Significance. If the quantitative conclusions hold, this is a useful step in connecting circumbinary discs to the depletion phenomenon and to post-AGB lifetimes and planetary-nebula formation. The paper has genuine strengths: it is the first to my knowledge to treat the time-dependent accretion from a viscous disc self-consistently in detailed MESA post-AGB models; it uses a homogeneous 58-star observational sample; it compares tracks in the observable Teff-[Zn/Ti] plane; and it includes explicit sensitivity tests for mixing depth (Fig. 15) and wind strength (Fig. 16). The qualitative mechanism, re-accretion of dust-free gas producing photospheric depletion, is supported by the models. The quantitative headline constraints, however, are conditional on two assumptions that the paper itself identifies as uncertain: the universal adopted composition of the accreted gas, and the adopted cool-wind mass-loss law. Because both assumptions affect the inferred accretion-rate and disc-mass thresholds, the significance of the stated constraints is lower than the abstract implies.

major comments (3)

[Sect. 3.2 and Fig. 2; Sect. 4.3]
[Sect. 4.2.1, Eq. (1), and Fig. 16]
[Sect. 4.1.1-4.1.2 and Tables A.1-A.2]

minor comments (4)

[Tables A.2 and A.1]
[Fig. 16 caption and Sect. 4.2.1]
[Sect. 4.2.2]
[Sect. 4.2 and marketplace statement]

Circularity Check

1 steps flagged · score 6.0 of 10

The saturated depletion pattern is the input accretion composition by construction; the accretion-rate and disc-mass constraints are independent forward-model results.

self definitional [Sect. 3.2, Figs. 2 and 3 (right panel); composition adopted for the MESA models in Sect. 4.2.2]
"In order to determine the chemical composition of the accreted material, we used the observed chemical abundances in depleted post-AGB objects as a basis. ... Since the abundances of the most refractory elements, such as Sc, are around −4 dex relative to solar, we take the accretion abundance of Ti to be −4 dex. ... fixing the abundance of Zn and Ti to 0 dex and −4 dex, respectively, yields the abundance pattern shown in Fig. 2. ... At this point, we retrieve the chemical composition of the accreted gas from Fig. 2."

The accreted-gas abundance pattern in Fig. 2 is not derived from first principles; it is calibrated to the most depleted observed post-AGB stars, with Ti fixed at −4 dex and Zn at 0 dex based on IRAS 11472-0800. The model's 'saturated' depletion pattern is obtained by diluting until the mixture converges to exactly this input composition, as the paper states: 'we retrieve the chemical composition of the accreted gas from Fig. 2.' The paper then identifies that saturated profile as similar to IRAS 11472-0800 and uses such patterns to argue that accretion reproduces the observed depletion. For the saturated and maximum-depletion level, this is a tautology: the model output is the empirical calibration by construction.

full rationale

The paper's central quantitative claim about accretion rates (≳ 3×10^-7 Msun/yr) and disc masses (∼ 10^-2 Msun) is a genuine forward-model constraint: a grid of MESA models with varying initial accretion rate, disc mass, and starting temperature is compared with observed stars in the Teff-[Zn/Ti] plane, and the requirement that model tracks reach the observed depletion values at low effective temperature is not an algebraic identity with the model inputs. The wind-strength sensitivity in Fig. 16 is a robustness concern about the adopted Schröder-Cuntz prescription, not a circularity. The same-author citation to Oomen et al. (2018) is used to exclude close-orbit stars and thereby favour high disc masses; it is load-bearing for the disc-mass conclusion, but it is a separately published empirical result, so it does not by itself create a self-referential loop. The genuinely circular element is the saturated depletion pattern: the maximum depletion level and the shape of the saturated abundance curve are predetermined by Fig. 2, which was calibrated from the most depleted stars. The paper is transparent about this limitation, but the step still reduces by construction, so the overall score is 6 rather than 0-2.

Assumptions & free parameters 7 free parameters · 7 assumptions · 0 invented entities

The modelling rests on several calibrated inputs. The most important is the chemical composition of the accreted gas, which is taken from the most depleted observed stars, so the saturated abundance pattern is an input rather than a prediction. The accretion rate and disc mass grids are constrained against the same sample, and the MESA tracks depend on mixing and wind assumptions that are only partially tested. No new physical entities are introduced.

free parameters (7)

Accreted gas abundance pattern = Ti at -4 dex, Zn at 0 dex, linear interpolation in condensation temperature
Set from the most depleted post-AGB stars (Fig. 2) and used as universal input to all dilution and MESA models; determines the saturated depletion pattern by construction.
Initial accretion rate onto the post-AGB star = Grid 5e-9 to 5e-7 Msun/yr; constrained to above about 3e-7 Msun/yr for luminous post-AGB stars
One of the two accretion-model parameters varied to match the observed sample; no independent measurement is used.
Initial disc mass = Grid 1e-3, 3e-3, and 1e-2 Msun; favoured value near 1e-2 Msun
Chosen within the observed range of post-AGB disc masses and constrained by requiring the models to reproduce depleted stars.
Accretion start temperature = 3500, 4000, 5000, and 6000 K
Mimics different binary separations and envelope masses at which re-accretion starts; affects how much depletion occurs before the star heats up.
Fraction of inflowing gas accreted by the post-AGB star = 0.5
Assumed half of the gas entering the binary cavity goes to the post-AGB star and half to the companion, following Farris et al. (2014); directly controls the disc drain time.
Mixing depth for accreted material = Down to the He II convection zone at about 80,000 K
Imposed in MESA to avoid an optically thick accreted layer; the paper tests alternative depths, but the main models use this ad hoc choice.
Disc model constants = alpha = 0.01, eta = 2, IL = 1, zeta = 0.1
Taken from Rafikov (2016b) for the viscous disc model; direct inputs to the initial viscous time and therefore to the accretion rate.

assumptions (7)

domain assumption Circumbinary discs around post-AGB binaries are formed by L2 mass loss and contain metal-poor gas because dust is removed by radiation pressure.
This is the mechanism under test, adopted from Waters et al. (1992) and related work; it is not derived in this paper.
domain assumption The Rafikov (2016b) viscous evolution equation for circumbinary disc accretion applies to post-AGB binaries.
Equation 3 is used as the physical basis for the time-dependent accretion rate, with constants taken from Rafikov (2016b).
domain assumption The post-AGB star can be modelled as a single star with accretion; binarity enters only through the accretion rate.
Section 6.1.1 assumes the star is detached and that any Roche-lobe overflow would be stable and only remove mass.
ad hoc to paper Accreted material is instantly mixed down to the He II convection zone in the 1D model.
Imposed in Sect. 4.2.2 and discussed in Sect. 6.1.3 to smooth the evolution; alternative mixing depths are only explored as a test.
domain assumption Post-AGB evolution depends only on current core mass, envelope mass, and thermal pulse phase, not on the initial model mass.
Section 6.1.2 tests initial masses and finds about 10% luminosity spread, which they argue does not affect the coarse mass binning.
domain assumption The post-AGB wind is described by the Schroeder-Cuntz (2005) RGB wind at low temperatures and the Miller Bertolami (2016) CSPN wind at high temperatures, with an arbitrary transition.
Section 4.2.1 states there is no better alternative and that the transition between log Teff = 3.7 and 3.9 is arbitrary; wind strength affects depletion at low masses.
domain assumption MESA version 10398 with the specified nuclear network and input physics is a faithful model of post-AGB evolution.
All model tracks rely on this code and configuration; no independent verification is provided.

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Pith. "Pith review of Modelling depletion by re-accretion of gas from a dusty disc in post-AGB stars." pith.science (2026). https://pith.science/paper/Q75JBCYP

@misc{pith2026190801788,
  author       = {Pith},
  title        = {Pith review of: Modelling depletion by re-accretion of gas from a dusty disc in post-AGB stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Q75JBCYP}},
  note         = {Machine review of arXiv:1908.01788}
}

abstract

Many disc-type post-asymptotic giant branch (post-AGB) stars are chemically peculiar, showing underabundances of refractory elements in their photospheres that correlate with condensation temperature. The aim of this paper is to investigate how accretion from a circumbinary disc can cause this phenomenon of depletion and how this impacts the evolution of post-AGB stars. We used the \texttt{MESA} code to evolve stars in the post-AGB phase, while including accretion of metal-poor gas. We compared the models to a sample of 58 observed disc-type post-AGB stars with chemical abundance data. For each of these stars, we estimated the luminosity and the mass using the Gaia distance. We modelled the accretion rate onto the binary from a viscously evolving disc for a range of initial accretion rates and disc masses. We find that large initial accretion rates ($\gtrsim 3\times10^{-7}$ $M_\odot$/yr) and large initial disc masses ($\sim10^{-2}$ $M_\odot$) are needed to reproduce the observed depleted post-AGB stars. Based on these high accretion rates, the evolution timescale of post-AGB stars can be significantly extended by a factor between two and five. We distinguish depletion patterns that are unsaturated (plateau profile) from those that are saturated, and we expect that post-red giant branch (post-RGB) stars are much more likely to show an unsaturated abundance pattern compared to post-AGB stars. Finally, because of the slower evolution of the low-mass post-RGB stars, we find that these systems can become depleted at lower effective temperatures ($< 5000$ K). We conclude that accretion from a circumbinary disc successfully accounts for the chemical peculiarity of post-AGB stars.

Figures

Figures reproduced from arXiv: 1908.01788 by the authors.

**Figure 1.** Depletion patterns of GZ Nor (Gezer et al. 2019) (left), IRAS 11472-0800 (Van Winckel et al. 2012) (middle), and IRAS 09144-4933 (Maas et al. 2005) (right). The abundances displayed are with respect to solar composition. There is some diversity in the shape of the patterns, but the general trend is a decrease of the element abundance with respect to condensation temperature. Condensation temperatures are taken from … view at source ↗

**Figure 2.** Estimate for chemical abundances of accreted gas. This is based on condensation temperatures of elements and the most depleted observed post-AGB stars. The abundances displayed are with respect to the initial composition of the star. Elements with higher condensation temperatures (Tcond) have lower accretion abundances. We use this chemical composition for the accreted gas in our MESA models. the abundance of Zn a… view at source ↗

**Figure 3.** Chemical abundances of a gas mixture after dilution of a solar-composition gas with abundances from [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

Figures from the paper (12 more)

**Figure 4.** Figure 4: Observed abundances of stars in our sample plotted in the [Zn/Ti]–[Fe/Ti] plane. The [Zn/Ti] tracer defines whether stars are depleted, while [Fe/Ti] distinguishes between saturated profiles and plateau profiles. Non-depleted objects are plotted as blue circles, platea…

**Figure 5.** Figure 5: Evolution of accretion rates over time from the accretion model of Eq. 5. Colours denote different initial accretion rates M˙ (0) in units of M /yr, while different linestyles represent different initial disc masses Md in units of M . Models with lower disc masses decr…

**Figure 6.** Figure 6: Two models of a 0.55-M star with different maximum depletion abundances. The evolution is plotted with respect to effective temperature of the star and the [Zn/Ti] ratio in the photosphere of the model. The blue curve with [Zn/Ti] = 4 dex is the accretion abundance fr…

**Figure 7.** Figure 7: Depletion and evolution timescales vs depletion value for a 0.55- M model for M˙ (0) = 1.5 × 10−8 , 5 × 10−8 , and 1.5 × 10−7 M /yr (top, middle, and bottom panel, respectively) with Md = 10−2 M and T0 = 4000 K. Orange solid lines show the evolution of the models in th…

**Figure 8.** Figure 8: shows all MESA models with a core mass of 0.40 M and initial accretion rates of 5 × 10−9 M /yr (upper panel) and 5 × 10−8 M /yr (lower panel). We show the models in terms of effective temperature and depletion value. The post-RGB stars that we assigned to the 0.40 M bi…

**Figure 9.** Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]

**Figure 7.** Figure 7: Several of the luminous post-AGB stars cannot be reproduced by our models. The four depleted stars to the left of the models in the lower panel of [PITH_FULL_IMAGE:figures/full_fig_p010_7.png]

**Figure 12.** Figure 12: Evolution of effective temperature over time of a 0.60 M postAGB star for different initial disc masses and an initial accretion rate of 5 × 10−7 M /yr. All 4 models start their evolution at an effective temperature of 4000 K. The blue solid line is a reference model…

**Figure 11.** Figure 11: Comparison between the observed depletion pattern and the best-fitting model for a plateau-type profile (top, EP Lyr) and a saturated-type profile (bottom, CC Lyr). Observed abundances of elements are given as blue circles, while abundances from the accretion model a…

**Figure 14.** Figure 14: Time evolution of depletion for post-RGB/AGB stars of different core masses. All the models have an initial accretion rate of 5 × 10−7 M /yr, an initial disc mass of 10−2 M , and start their evolution at 4000 K. stars to have such a profile. Only 2 out of 18 stars c…

**Figure 15.** Figure 15: Comparison of 0.55-M models with 1.5×10−7 M /yr initial accretion rate for different assumptions on the depth of mixing. The left panel shows models where accreted gas is only mixed with the outermost convective zone. The middle panel shows mixing down to the He ii co…

**Figure 16.** Figure 16: Comparison of 0.55-M models with 5×10−8 M /yr initial accretion rate for different stellar-wind strengths. The left panel shows models with the normal wind strength used throughout this work. The middle panel shows models with a stellar wind that is weaker by a factor…

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Works this paper leans on

70 extracted references · 47 canonical work pages · cited by 1 Pith paper

[1]

& Lubow, S

Artymowicz, P. & Lubow, S. H. 1994, ApJ, 421, 651

1994
[2]

J., & Scott, P

Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481

2009
[3]

2010, Mem

Ayres, T. 2010, Mem. Soc. Astron. Italiana, 81, 553

work page 2010
[4]

Bailer-Jones, C. A. L., Rybizki, J., Fouesneau, M., Mantelet, G., & Andrae, R. 2018, AJ, 156, 58 Blöcker, T. 1995, A&A, 299, 755

work page 2018
[5]

2017, A&A, 607, A60

Bollen, D., Van Winckel, H., & Kamath, D. 2017, A&A, 607, A60

work page 2017
[6]

2013, A&A, 557, A104

Carrizo, A. 2013, A&A, 557, A104

work page 2013
[7]

A., Clayton, G

Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245

1989
[8]

Cranmer, S. R. & Saar, S. H. 2011, ApJ, 741, 54 De Marco, O. & Izzard, R. G. 2017, PASA, 34, 1 De Ruyter, S., Van Winckel, H., Maas, T., et al. 2006, A&A, 448, 641 De Smedt, K., Van Winckel, H., Kamath, D., et al. 2016, A&A, 587, A6 D’Orazio, D. J., Haiman, Z., & MacFadyen, A. 2013, MNRAS, 436, 2997

work page 2011

Show all 70 references

[9]

D., Duﬀell, P., MacFadyen, A

Farris, B. D., Duﬀell, P., MacFadyen, A. I., & Haiman, Z. 2014, ApJ, 783, 134

2014
[10]

& Jorissen, A

Frankowski, A. & Jorissen, A. 2007, Baltic Astronomy, 16, 104 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, A1

2007
[11]

A., & Miller Bertolami, M

Gesicki, K., Zijlstra, A. A., & Miller Bertolami, M. M. 2018, Nature Astronomy, 2, 580

2018
[12]

2015, MNRAS, 453, 133

Gezer, I., Van Winckel, H., Bozkurt, Z., et al. 2015, MNRAS, 453, 133

2015
[13]

2019, MNRAS, 1918

Gezer, I., Van Winckel, H., Manick, R., & Kamath, D. 2019, MNRAS, 1918

2019
[14]

L., & Gonzalez, G

Giridhar, S., Lambert, D. L., & Gonzalez, G. 1998, ApJ, 509, 366

1998
[15]

L., & Gonzalez, G

Giridhar, S., Lambert, D. L., & Gonzalez, G. 2000, ApJ, 531, 521

2000
[16]

L., Reddy, B

Giridhar, S., Lambert, D. L., Reddy, B. E., Gonzalez, G., & Yong, D. 2005, ApJ, 627, 432

2005
[17]

K., & Lambert, D

Giridhar, S., Rao, N. K., & Lambert, D. L. 1994, ApJ, 437, 476

1994
[18]

& Wallerstein, G

Gonzalez, G. & Wallerstein, G. 1996, MNRAS, 280, 515

1996
[19]

2012, A&A, 542, A27

Gorlova, N., Van Winckel, H., Gielen, C., et al. 2012, A&A, 542, A27

2012
[20]

P., et al

Gorlova, N., Van Winckel, H., Ikonnikova, N. P., et al. 2015, MNRAS, 451, 2462

2015
[21]

L., Menu, J., et al

Hillen, M., de Vries, B. L., Menu, J., et al. 2015, A&A, 578, A40

2015
[22]

2016, A&A, 588, L1

Hillen, M., Kluska, J., Le Bouquin, J.-B., et al. 2016, A&A, 588, L1

2016
[23]

2014, A&A, 568, A12

Hillen, M., Menu, J., Van Winckel, H., et al. 2014, A&A, 568, A12

2014
[24]

2017, A&A, 599, A41

Hillen, M., Van Winckel, H., Menu, J., et al. 2017, A&A, 599, A41

2017
[25]

Horowitz, D. H. 1986, Journal of the American Association of Variable Star Observers (JAA VSO), 15, 223

1986
[26]

J., Van Winckel, H., Reyniers, M., et al

Hrivnak, B. J., Van Winckel, H., Reyniers, M., et al. 2008, AJ, 136, 1557

2008
[27]

& Jermyn, A

Izzard, R. & Jermyn, A. 2018, Galaxies, 6, 97 Article number, page 15 of 20 A&A proofs: manuscript no. depletionpaper Jofré, P., Heiter, U., & Soubiran, C. 2018, arXiv e-prints [arXiv:1811.08041]

2018 arXiv
[28]

& Boﬃn, H

Jones, D. & Boﬃn, H. M. J. 2017, Nature Astronomy, 1, 0117

2017
[29]

R., & Van Winckel, H

Kamath, D., Wood, P. R., & Van Winckel, H. 2014, MNRAS, 439, 2211

2014
[30]

R., & Van Winckel, H

Kamath, D., Wood, P. R., & Van Winckel, H. 2015, MNRAS, 454, 1468

2015
[31]

R., Van Winckel, H., & Nie, J

Kamath, D., Wood, P. R., Van Winckel, H., & Nie, J. D. 2016, A&A, 586, L5

2016
[32]

2011, Baltic Astronomy, 20, 65

Kipper, T. 2011, Baltic Astronomy, 20, 65

2011
[33]

2013, Baltic Astronomy, 22, 101

Kipper, T. 2013, Baltic Astronomy, 22, 101

2013
[34]

2018, A&A, 616, A153

Kluska, J., Hillen, M., Van Winckel, H., et al. 2018, A&A, 616, A153

2018
[35]

2019, A&A, 624, A60

Laverick, M., Lobel, A., Royer, P., et al. 2019, A&A, 624, A60

2019
[36]

R., Huber, D., et al

Li, T., Bedding, T. R., Huber, D., et al. 2018, MNRAS, 475, 981

2018
[37]

2018, A&A, 616, A2

Lindegren, L., Hernández, J., Bombrun, A., et al. 2018, A&A, 616, A2

2018
[38]

Linsky, J. L. & Haisch, B. M. 1979, ApJ, 229, L27

1979
[39]

2003, ApJ, 591, 1220

Lodders, K. 2003, ApJ, 591, 1220

2003
[40]

Luri, X., Brown, A. G. A., Sarro, L. M., et al. 2018, A&A, 616, A9

2018
[41]

Maas, T., Giridhar, S., & Lambert, D. L. 2007, ApJ, 666, 378

2007
[42]

2005, A&A, 429, 297

Maas, T., Van Winckel, H., & Lloyd Evans, T. 2005, A&A, 429, 297

2005
[43]

2003, A&A, 405, 271

Maas, T., Van Winckel, H., Lloyd Evans, T., et al. 2003, A&A, 405, 271

2003
[44]

2002, A&A, 386, 504

Maas, T., Van Winckel, H., & Waelkens, C. 2002, A&A, 386, 504

2002
[45]

MacFadyen, A. I. & Milosavljevi´c, M. 2008, ApJ, 672, 83

2008
[46]

2019, arXiv e-prints, arXiv:1906.10492

Manick, R., Kamath, D., Van Winckel, H., et al. 2019, arXiv e-prints, arXiv:1906.10492

2019 arXiv
[47]

2017, A&A, 597, A129

Manick, R., Van Winckel, H., Kamath, D., Hillen, M., & Escorza, A. 2017, A&A, 597, A129

2017
[48]

Marigo, P., Girardi, L., Weiss, A., Groenewegen, M. A. T., & Chiosi, C. 2004, A&A, 423, 995 Men’shchikov, A. B., Schertl, D., Tuthill, P. G., Weigelt, G., & Yungelson, L. R. 2002, A&A, 393, 867 Miller Bertolami, M. M. 2016, A&A, 588, A25

2004
[49]

2018, A&A, 620, A85

Oomen, G.-M., Van Winckel, H., Pols, O., et al. 2018, A&A, 620, A85

2018
[50]

2011, ApJS, 192, 3

Paxton, B., Bildsten, L., Dotter, A., et al. 2011, ApJS, 192, 3

2011
[51]

2013, ApJS, 208, 4

Paxton, B., Cantiello, M., Arras, P., et al. 2013, ApJS, 208, 4

2013
[52]

2015, ApJS, 220, 15

Paxton, B., Marchant, P., Schwab, J., et al. 2015, ApJS, 220, 15

2015
[53]

B., et al

Paxton, B., Schwab, J., Bauer, E. B., et al. 2018, ApJS, 234, 34

2018
[54]

D., & Tomida, K

Pejcha, O., Metzger, B. D., & Tomida, K. 2016, MNRAS, 461, 2527

2016
[55]

Pollard, K. H. & Cottrell, P. L. 1995, in ASP Conf. Ser. 83: IAU Colloq. 155: Astrophysical Applications of Stellar Pulsation, 409–+

1995
[56]

Pringle, J. E. 1991, MNRAS, 248, 754 Raﬁkov, R. R. 2016a, ApJ, 830, 7 Raﬁkov, R. R. 2016b, ApJ, 830, 8

1991
[57]

Rao, S. S. & Giridhar, S. 2014, Rev. Mexicana Astron. Astroﬁs., 50, 49

2014
[58]

S., Giridhar, S., & Lambert, D

Rao, S. S., Giridhar, S., & Lambert, D. L. 2012, MNRAS, 419, 1254

2012
[59]

1975, Memoires of the Societe Royale des Sciences de Liege, 8, 369

Reimers, D. 1975, Memoires of the Societe Royale des Sciences de Liege, 8, 369

1975
[60]

1989, in IAU Symposium, V ol

Renzini, A. 1989, in IAU Symposium, V ol. 131, Planetary Nebulae, ed. S. Torres- Peimbert, 391–400

1989
[61]

A., & Lèbre, A

Sabin, L., Wade, G. A., & Lèbre, A. 2015, MNRAS, 446, 1988 Schröder, K.-P. & Cuntz, M. 2005, ApJ, 630, L73 Schröder, K.-P. & Cuntz, M. 2007, A&A, 465, 593

2015
[62]

& Krolik, J

Shi, J.-M. & Krolik, J. H. 2015, ApJ, 807, 131

2015
[63]

H., Lubow, S

Shi, J.-M., Krolik, J. H., Lubow, S. H., & Hawley, J. F. 2012, ApJ, 749, 118

2012
[64]

H., Lubow, S

Shu, F. H., Lubow, S. H., & Anderson, L. 1979, ApJ, 229, 223

1979
[65]

H., et al

Tayar, J., Somers, G., Pinsonneault, M. H., et al. 2017, ApJ, 840, 17 van Winckel, H. 1995, PhD thesis, KU Leuven Van Winckel, H. 1997, A&A, 319, 561 Van Winckel, H. 2003, ARA&A, 41, 391 Van Winckel, H. 2017, in IAU Symposium, V ol. 323, Planetary Nebulae: Multi-Wavelength Pro...

2017
[66]

& Wood, P

Vassiliadis, E. & Wood, P. R. 1994, ApJS, 92, 125

1994
[67]

Waelkens, C., Lamers, H. J. G. L. M., Waters, L. B. F. M., et al. 1991, A&A, 242, 433

1991
[68]

Waelkens, C., Van Winckel, H., Waters, L. B. F. M., & Bakker, E. J. 1996, A&A, 314, L17

1996
[69]

Waters, L. B. F. M., Trams, N. R., & Waelkens, C. 1992, A&A, 262, L37

1992
[70]

& Ferguson, J

Weiss, A. & Ferguson, J. W. 2009, A&A, 508, 1343 Article number, page 16 of 20 Oomen et al.: Modelling depletion by re-accretion of gas from a dusty disc in post-AGB stars Appendix A: Observational data In this appendix we present the observational data collected from literatu...

2018

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.

[1] [1]

& Lubow, S

Artymowicz, P. & Lubow, S. H. 1994, ApJ, 421, 651

1994

[2] [2]

J., & Scott, P

Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481

2009

[3] [3]

2010, Mem

Ayres, T. 2010, Mem. Soc. Astron. Italiana, 81, 553

work page 2010

[4] [4]

Bailer-Jones, C. A. L., Rybizki, J., Fouesneau, M., Mantelet, G., & Andrae, R. 2018, AJ, 156, 58 Blöcker, T. 1995, A&A, 299, 755

work page 2018

[5] [5]

2017, A&A, 607, A60

Bollen, D., Van Winckel, H., & Kamath, D. 2017, A&A, 607, A60

work page 2017

[6] [6]

2013, A&A, 557, A104

Carrizo, A. 2013, A&A, 557, A104

work page 2013

[7] [7]

A., Clayton, G

Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245

1989

[8] [8]

Cranmer, S. R. & Saar, S. H. 2011, ApJ, 741, 54 De Marco, O. & Izzard, R. G. 2017, PASA, 34, 1 De Ruyter, S., Van Winckel, H., Maas, T., et al. 2006, A&A, 448, 641 De Smedt, K., Van Winckel, H., Kamath, D., et al. 2016, A&A, 587, A6 D’Orazio, D. J., Haiman, Z., & MacFadyen, A. 2013, MNRAS, 436, 2997

work page 2011