Marie Van de Sande

Scopus Publications

Sense and sensitivity-I. Uncertainty analysis of the gas-phase chemistry in AGB outflows
M Van de Sande, M Gueguen, T Danilovich, T J Millar
Monthly Notices of the Royal Astronomical Society, 2026
Chemical reaction networks are central to all chemical models. Each rate coefficient has an associated uncertainty, which is generally not taken into account when calculating the chemistry. We performed the first uncertainty analysis of a chemical model of C- and O-rich asymptotic giant branch (AGB) outflows using the Rate22 reaction network. Quantifying the error on the model predictions enables us to determine the need for adding complexity to the model. Using a Monte Carlo sampling method, we quantified the impact of the uncertainties on the chemical kinetic data on the predicted fractional abundances and column densities. The errors are caused by a complex interplay of reactions forming and destroying each species. Parent species show an error on their envelope sizes, which is not caused by the uncertainty on their photodissociation rate, but rather the chemistry reforming the parent after its photodissociation. Using photodissociation models to estimate the envelope size might be an oversimplification. The error on the CO envelope impacts retrieved mass-loss rates by up to a factor of two. For daughter species, the error on the peak fractional abundance ranges from a factor of a few to three orders of magnitude, and is on average about 10 per cent of its value. This error is positively correlated with the error on the column density. The standard model suffices for many species, e.g. the radial distribution of cyanopolyynes and hydrocarbon radicals around IRC +10216. However, including spherical asymmetries, dust-gas chemistry, and photochemistry induced by a close-by stellar companion are still necessary to explain certain observations.
Evidence for the Keplerian orbit of a close companion around a giant star
Mats Esseldeurs, Leen Decin, Joris De Ridder, Yoshiya Mori, Amanda I. Karakas, Jolien Malfait, Taíssa Danilovich, Stéphane Mathis, Anita M. S. Richards, Raghvendra Sahai, Jeremy Yates, Marie Van de Sande, Maarten Baes, Alain Baudry, Jan Bolte, Thomas Ceulemans, Frederik De Ceuster, Ileyk El Mellah, Sandra Etoka, Carl Gottlieb, Fabrice Herpin, Pierre Kervella, Camille Landri, Louise Marinho, Iain McDonald, Karl Menten, Tom Millar, Zara Osborn, Bannawit Pimpanuwat, John Plane, Daniel J. Price, Lionel Siess, Owen Vermeulen, Ka Tat Wong
Nature Astronomy, 2026
ATOMIUM: Continuum emission and evidence of dust enhancement from binary motion
T. Danilovich, N. Samaratunge, Y. L. Mori, A. M. S. Richards, A. Baudry, S. Etoka, M. Montargès, P. Kervella, I. McDonald, C. A. Gottlieb, A. Wallace, D. J. Price, L. Decin, J. Bolte, T. Ceulemans, F. De Ceuster, A. de Koter, D. Dionese, I. El Mellah, M. Esseldeurs, M. Gray, F. Herpin, T. Khouri, E. Lagadec, C. Landri, L. Marinho, K. M. Menten, T. J. Millar, H. S. P. Müller, B. Pimpanuwat, J. M. C. Plane, R. Sahai, L. Siess, M. Van de Sande, O. Vermeulen, K. T. Wong, J. Yates, A. Zijlstra
Astronomy and Astrophysics, 2025
Context. Low- and intermediate-mass stars on the asymptotic giant branch (AGB) account for a significant portion of the dust and chemical enrichment in their host galaxy. Understanding the dust formation process of these stars and their more massive counterparts, the red supergiants, is essential for quantifying galactic chemical evolution. Aims. To improve our understanding of the dust nucleation and growth process, we aim to better constrain stellar properties at millimetre wavelengths. To characterise how this process varies with the mass-loss rate and pulsation period, we studied a sample of oxygen-rich and S-type evolved stars. Methods. Here we present ALMA observations of the continuum emission around a sample of 17 stars from the ATOMIUM survey. We analysed the stellar parameters at 1.24 mm and the dust distributions at high angular resolutions. Results. From our analysis of the stellar contributions to the continuum flux, we find that the semi-regular variables all have smaller physical radii and fainter monochromatic luminosities than the Mira variables. Comparing these properties with pulsation periods, we find a positive trend between the stellar radius and period only for the Mira variables with periods of more than 300 days, and we find and a positive trend between the period and the monochromatic luminosity only for the red supergiants and the most extreme AGB stars with periods of more than 500 days. We find that the continuum emission at 1.24 mm can be classified into four groups; (i) ‘featureless’ continuum emission is confined to the (unresolved) regions close to the star for five stars in our sample, (ii) relatively uniform extended flux is seen for four stars, (iii) tentative elongated features are seen for three stars, and (iv) the remaining five stars have unique or unusual morphological features in their continuum maps. These features can be explained by the fact that 10 of the 14 AGB stars in our sample have binary companions. Conclusions. Based on our results, we conclude that there are two modes of dust formation: well-established pulsation-enhanced dust formation and our newly proposed companion-enhanced dust formation. If the companion is located close to the AGB star, in the wind acceleration region, then additional dust formed in the wake of the companion can increase the amount of mass lost through the dust-driven wind. This explains the different dust morphologies seen around our stars and partly accounts for the large scatter in literature mass-loss rates, especially among semi-regular stars with small pulsation periods.
Charting circumstellar chemistry of carbon-rich asymptotic giant branch stars: II. Abundances and spatial distributions of CS
R. Unnikrishnan, M. Andriantsaralaza, E. De Beck, L.-Å. Nyman, H. Olofsson, et al.
Astronomy and Astrophysics, 2025
Context . The circumstellar envelopes (CSEs) of asymptotic giant branch (AGB) stars harbour a rich variety of molecules and are sites of complex chemistry. Our current understanding of the circumstellar chemical processes of carbon-rich AGB stars is predominantly based on observations of a single star, IRC +10 216, often regarded as an archetypical carbon star. Aims . We aim to estimate stellar and circumstellar properties for five carbon stars, and constrain their circumstellar CS abundances. This study compares the CS abundances among the sources, informs circumstellar chemical models, and helps to assess if IRC+10 216 is a good representative of the physics and chemistry of carbon star CSEs. Methods . We modelled the spectral energy distributions (SEDs) and CO line emission to derive the stellar and outflow properties. Using these, we then retrieved CS abundance profiles with detailed radiative transfer modelling, imposing spatial and excitation constraints from ALMA and single-dish observations. Results . We obtain good fits to the SEDs and CO lines for all sources and reproduce the CS line emission across various transitions and apertures, yielding robust estimates of the CS abundance profiles. Peak CS fractional abundances range from 1×10 −6 −4×10 −6 , with e-folding radii of 1.8×10 16 −6.8×10 16 cm. We also derive reliable 12 C/ 13 C and 32 S/ 34 S ratios from CS isotopologue modelling. Conclusions . Our results refine previous single-dish CS abundance estimates and improve the relative uncertainty on the CS e-folding radius for IRAS 07454-7112 by a factor of ~2.5. Chemical models reproduce our estimates of the CS radial extent, corroborating the CS photodissociation framework used therein. We find no significant differences between the derived CS abundance profiles for IRC +10 216 and the rest of the sample, apart from the expected density-driven variations.
An accreting dwarf star orbiting the S-type giant star π1 Gru
M. Montargès, J. Malfait, M. Esseldeurs, A. de Koter, F. Baron, P. Kervella, T. Danilovich, A. M. S. Richards, R. Sahai, I. McDonald, T. Khouri, S. Shetye, A. Zijlstra, M. Van de Sande, I. El Mellah, F. Herpin, L. Siess, S. Etoka, D. Gobrecht, L. Marinho, S. H. J. Wallström, K. T. Wong, J. Yates
Astronomy and Astrophysics, 2025
Context. At the end of their lives, low- to intermediate-mass stars reach the asymptotic giant branch (AGB), during which their photospheres expand by up to several hundred times and strong stellar winds develop. These changes lead to various interactions with celestial bodies in their close circumstellar environments, including mass- and angular-momentum transfer. Aims. We aim to characterize the properties of the inner companion of the S-type AGB star π1 Gru and to identify plausible future evolutionary scenarios for this triple system. Methods. We observed π1 Gru with the Atacama Large Millimeter/sub-millimeter Array (ALMA) and the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument of the Very Large Telescope (VLT), collected archival photometric data, and used the HIPPARCOS-Gaia proper motion anomaly. We derived the best orbital parameters using Bayesian inference. Results. In June-July 2019, the inner companion, π1 Gru C, was located at 37.4±2.0 mas from the primary (a projected separation of 6.05±0.55 au at 161.7±11.7 pc). The best orbital solution yields a companion mass of 0.86+0.22−0.20 M⊙ (using the derived mass of the primary) and a semi-major axis of 7.05−0.57+0.54 au, corresponding to an orbital period of 11.0−1.5+1.7 yr. The preferred solution is an elliptical orbit with eccentricity e = 0.35−0.17+0.18, although a circular orbit cannot be fully excluded. The close companion could be either a K1VK7VF9.5V star or a white dwarf (WD). Ultraviolet and millimeter continuum photometry are consistent with the presence of an accretion disk around the close companion. The ultraviolet emission may originate from hot spots in an overall cooler disk, or from a hot disk if the companion is a WD. Conclusions. Although the close companion and the AGB star are interacting and an accretion disk is observed around the companion, the mass-accretion rate is too low to trigger a Type Ia supernova, but it could produce novæevery ≈900 yr. Short-wavelength, spatially resolved observations are required to further constrain the nature of the C companion. Searches for close-in companions similar to this system will improve our understanding of the physics of mass and angular momentum transfer, as well as orbital evolution during late evolutionary stages.
The salty emission of the intermediate-mass AGB star OH 30.1-0.7
T Danilovich, A M S Richards, M Van de Sande, C A Gottlieb, T J Millar, A I Karakas, H S P Müller, K Justtanont, J M C Plane, S Etoka, S H J Wallström, L Decin, D Engels, M A T Groenewegen, F Kerschbaum, T Khouri, A de Koter, H Olofsson, C Paladini, R J Stancliffe
Monthly Notices of the Royal Astronomical Society, 2025
We analyse continuum and molecular emission, observed with Atacama Large Millimetre/submillimetre Array, from the dust-enshrouded intermediate-mass asymptotic giant branch (AGB) star OH 30.1−0.7. We find a secondary peak in the continuum maps, ‘feature B’, separated by 4.6 arcsec from the AGB star, which corresponds to a projected separation of $1.8\\times 10^{4}$ au, placing a lower limit on the physical separation. This feature is most likely composed of cold dust and is likely to be ejecta associated with the AGB star, though we cannot rule out that it is a background object. The molecular emission we detect includes lines of CO, SiS, CS, $\\mathrm{SO}_2$, NS, NaCl, and KCl. We find that the NS emission is off centre and arranged along an axis perpendicular to the direction of feature B, indicative of a UV-emitting binary companion (e.g. a G-type main sequence star or hotter), perhaps on an eccentric orbit, contributing to its formation. However, the NaCl and KCl emission constrain the nature of that companion to not be hotter than a late B-type main-sequence star. We find relatively warm emission arising from the inner wind and detect several vibrationally excited lines of SiS ($\\upsilon =1$), NaCl (up to $\\upsilon =4$), and KCl (up to $\\upsilon =2$), and emission from low-energy levels in the mid to outer envelope, as traced by $\\mathrm{SO}_2$. The CO emission is abruptly truncated around 3.5 arcsec or 14 000 au from the continuum peak, suggesting that mass loss at a high rate may have commenced as little as 2800 yr ago.
Experimental and Theoretical Investigation of the Reaction of C2H with Formaldehyde (CH2O) at Very Low Temperatures and Application to Astrochemical Models
Kevin M. Douglas, Niclas A. West, Daniel I. Lucas, Marie Van de Sande, Mark A. Blitz, Dwayne E. Heard
ACS Earth and Space Chemistry, 2024
Rate coefficients for the reaction of C2H with CH2O were measured for the first time over the temperature range of 37–603 K, with the C2H radicals produced by pulsed laser photolysis and detected by CH radical chemiluminescence following their reaction with O2. The low temperature measurements (≤93 K) relevant to the interstellar medium were made within a Laval nozzle gas expansion, while higher temperature measurements (≥308 K) were made within a temperature controlled reaction cell. The rate coefficients display a negative temperature dependence below 300 K, reaching (1.3 ± 0.2) × 10–10 cm3 molecule–1 s–1 at 37 K, while only a slight positive temperature dependence is observed at higher temperatures above 300 K. Ab initio calculations of the potential energy surface (PES) were combined with rate theory calculations using the MESMER master-equation program in order to predict rate coefficients and branching ratios. The three lowest energy entrance channels on the PES all proceed via the initial formation of a weakly bound prereaction complex, bound by ∼5 kJ mol–1, followed by either a submerged barrier on the route to the H-abstraction products (C2H2 + CHO), or emerged barriers on the routes to the C- or O-addition species. MESMER calculations indicated that over the temperature range investigated (10–600 K) the two addition channels were uncompetitive, accounting for less 0.3% of the total product yield even at 600 K. The PES containing only the H-abstraction product channel was fit to the experimentally determined rate coefficients, with only a minor adjustment to the height of the submerged barrier (from −2.6 to −5.9 kJ mol–1) required. Using this new submerged barrier height, and including the subsequent dissociation of the CHO product into CO + H in the PES, rate coefficients and branching ratios were calculated over a wide range of temperatures and pressures and these used to recommend best-fit modified Arrhenius expressions for use in astrochemical modeling. Inclusion of the new rate coefficients and branching ratios in a UMIST chemical model of an outflow from an asymptotic giant branch (AGB) star yielded no significant changes in the abundances of the reactants or the products of the reaction, however, removal of the C-addition channel currently in the UMIST Rate22 database did result in a significant reduction in the abundance of propynal (HCCCHO).
Hybrid approach predicts a lower binding energy for benzene on water ice
Victoria H J Clark, David M Benoit, Marie Van de Sande, Catherine Walsh
Monthly Notices of the Royal Astronomical Society, 2024
In this paper, we provide a highly accurate value for the binding energy of benzene to proton-ordered crystalline water ice (XIh), as a model for interstellar ices. We compare our computed value to the latest experimental data available from temperature-programmed desorption experiments and find that our binding energy value agrees well with data obtained from binding to either crystalline or amorphous ice. Importantly, our new value is lower than that used in most astrochemical networks by about nearly half its value. We explore the impact of this revised binding energy value for both an asymptotic giant branch (AGB) outflow and a protoplanetary disc. We find that the lower value of the binding energy predicted here compared with values used in the literature (4050 K versus 7587 K) leads to less depletion of gas-phase benzene in an AGB outflow, and leads to a shift outwards in the benzene snowline in the mid-plane of a protoplanetary disc. Using this new value, the AGB model predicts lower abundances of benzene in the solid phase throughout the outflow. The disc model also predicts a larger reservoir of gas-phase benzene in the inner disc, which is consistent with the recent detections of benzene for the first time in protoplanetary discs with JWST.
MACE: A Machine-learning Approach to Chemistry Emulation
Silke Maes, Frederik De Ceuster, Marie Van de Sande, Leen Decin
Astrophysical Journal, 2024
The chemistry of an astrophysical environment is closely coupled to its dynamics, the latter often found to be complex. Hence, to properly model these environments a 3D context is necessary. However, solving chemical kinetics within a 3D hydro simulation is computationally infeasible for even a modest parameter study. In order to develop a feasible 3D hydro-chemical simulation, the classical chemical approach needs to be replaced by a faster alternative. We present mace, a Machine-learning Approach to Chemistry Emulation, as a proof-of-concept work on emulating chemistry in a dynamical environment. Using the context of AGB outflows, we have developed an architecture that combines the use of an autoencoder (to reduce the dimensionality of the chemical network) and a set of latent ordinary differential equations (that are solved to perform the temporal evolution of the reduced features). Training this architecture with an integrated scheme makes it possible to successfully reproduce a full chemical pathway in a dynamical environment. mace outperforms its classical analog on average by a factor of 26. Furthermore, its efficient implementation in PyTorch results in a sublinear scaling with respect to the number of hydrodynamical simulation particles.
Modelling predicts a molecule-rich disc around the AGB star L2 Puppis
M Van de Sande, C Walsh, T Danilovich, F De Ceuster, T Ceulemans
Monthly Notices of the Royal Astronomical Society, 2024
The nearby oxygen-rich AGB star L$_2$ Pup hosts a well-studied nearly edge-on disc. To date, discs around AGB stars have not been chemically studied in detail. By combining a parametrization commonly used for protoplanetary discs and archival ALMA observations, we retrieved an updated density and temperature structure of this disc. This physical model was then used as input to the first chemical model of an AGB disc. The model shows that the physical structure of the disc has a large impact on its chemistry, with certain species showing large changes in column density relative to a radial outflow, indicating that chemistry could be used as a tracer of discs that cannot be directly imaged. Despite its oxygen-rich nature, the daughter species formed within the disc are surprisingly carbon-rich. Two chemical regimes can be distinguished: cosmic-ray induced chemistry in the midplane and photochemistry induced by the interstellar radiation field in the outer regions. Certain complex organic molecules are formed in the midplane. This occurs via gas-phase chemistry only, as the disc is too warm for dust-gas chemistry. The photochemistry in the outer regions leads to the efficient formation of (long) carbon-chains. The predictions of the model allow us to tentatively put the disc’s age $\\lesssim 10^5$ yr. Additional observations are necessary to better constrain the physical structure of L$_2$ Pup’s disc and are essential to test the predictions made by the chemical model. Our exploratory work paves the way for a more general study of the chemistry of AGB discs.
Chemical tracers of a highly eccentric AGB–main-sequence star binary
T. Danilovich, J. Malfait, M. Van de Sande, M. Montargès, P. Kervella, F. De Ceuster, A. Coenegrachts, T. J. Millar, A. M. S. Richards, L. Decin, C. A. Gottlieb, C. Pinte, E. De Beck, D. J. Price, K. T. Wong, J. Bolte, K. M. Menten, A. Baudry, A. de Koter, S. Etoka, D. Gobrecht, M. Gray, F. Herpin, M. Jeste, E. Lagadec, S. Maes, I. McDonald, L. Marinho, H. S. P. Müller, B. Pimpanuwat, J. M. C. Plane, R. Sahai, S. H. J. Wallström, J. Yates, A. Zijlstra
Nature Astronomy, 2024
The UMIST Database for Astrochemistry 2022
T. J. Millar, C. Walsh, M. Van de Sande, A. J. Markwick
Astronomy and Astrophysics, 2024
ATOMIUM: Molecular inventory of 17 oxygen-rich evolved stars observed with ALMA
S. H. J. Wallström, T. Danilovich, H. S. P. Müller, C. A. Gottlieb, S. Maes, M. Van de Sande, L. Decin, A. M. S. Richards, A. Baudry, J. Bolte, T. Ceulemans, F. De Ceuster, A. de Koter, I. El Mellah, M. Esseldeurs, S. Etoka, D. Gobrecht, E. Gottlieb, M. Gray, F. Herpin, M. Jeste, D. Kee, P. Kervella, T. Khouri, E. Lagadec, J. Malfait, L. Marinho, I. McDonald, K. M. Menten, T. J. Millar, M. Montargès, J. A. Nuth, J. M. C. Plane, R. Sahai, L. B. F. M. Waters, K. T. Wong, J. Yates, A. Zijlstra
Astronomy and Astrophysics, 2024
MELCHIORS: The Mercator Library of High Resolution Stellar Spectroscopy
P. Royer, T. Merle, K. Dsilva, S. Sekaran, H. Van Winckel, Y. Frémat, M. Van der Swaelmen, S. Gebruers, A. Tkachenko, M. Laverick, M. Dirickx, G. Raskin, H. Hensberge, M. Abdul-Masih, B. Acke, M. L. Alonso, S. Bandhu Mahato, P. G. Beck, N. Behara, S. Bloemen, B. Buysschaert, N. Cox, J. Debosscher, P. De Cat, P. Degroote, R. De Nutte, K. De Smedt, B. de Vries, L. Dumortier, A. Escorza, K. Exter, S. Goriely, N. Gorlova, M. Hillen, W. Homan, A. Jorissen, D. Kamath, M. Karjalainen, R. Karjalainen, P. Lampens, A. Lobel, R. Lombaert, P. Marcos-Arenal, J. Menu, F. Merges, E. Moravveji, P. Nemeth, P. Neyskens, R. Ostensen, P. I. Pápics, J. Perez, S. Prins, S. Royer, A. Samadi-Ghadim, H. Sana, A. Sans Fuentes, S. Scaringi, V. Schmid, L. Siess, C. Siopis, K. Smolders, Á. Sódor, A. Thoul, S. Triana, B. Vandenbussche, M. Van de Sande, G. Van De Steene, S. Van Eck, P. A. M. van Hoof, A. J. Van Marle, T. Van Reeth, L. Vermeylen, D. Volpi, J. Vos, C. Waelkens
Astronomy and Astrophysics, 2024
Computational astrochemistry: general discussion
Stefan T. Bromley, Sandra Brünken, Cecilia Ceccarelli, Martin Cordiner, Kristen Darnell, Gwenaëlle Dufour, Athena Flint, Robin T. Garrod, Murthy S. Gudipati, Joshua Halpern, Eric Herbst, Ko-Yun Huang, Inga Kamp, Nikku Madhusudhan, Martin R. S. McCoustra, Arthur G. Suits, Marie Van de Sande, Ewine F. van Dishoeck, Serena Viti, Laurent Wiesenfeld
Faraday Discussions, 2023
Sensitivity study of chemistry in AGB outflows using chemical kinetics
S Maes, M Van de Sande, T Danilovich, F De Ceuster, L Decin
Monthly Notices of the Royal Astronomical Society, 2023
Disentangling physics and chemistry in AGB outflows: revealing degeneracies when adding complexity
Marie Van de Sande, Catherine Walsh, Tom J. Millar
Faraday Discussions, 2023
The VLT/SPHERE view of the A TOMIUM cool evolved star sample: I. Overview: Sample characterization through polarization analysis
M. Montargès, E. Cannon, A. de Koter, T. Khouri, E. Lagadec, P. Kervella, L. Decin, I. McDonald, W. Homan, L. B. F. M. Waters, R. Sahai, C. A. Gottlieb, J. Malfait, S. Maes, B. Pimpanuwat, M. Jeste, T. Danilovich, F. De Ceuster, M. Van de Sande, D. Gobrecht, S. H. J. Wallström, K. T. Wong, I. El Mellah, J. Bolte, F. Herpin, A. M. S. Richards, A. Baudry, S. Etoka, M. D. Gray, T. J. Millar, K. M. Menten, H. S. P. Müller, J. M. C. Plane, J. Yates, A. Zijlstra
Astronomy and Astrophysics, 2023
Experimental and theoretical study of the low-temperature kinetics of the reaction of CN with CH2O and implications for interstellar environments
Niclas A. West, Lok Hin Desmond Li, Tom J. Millar, Marie Van de Sande, Edward Rutter, Mark A. Blitz, Julia H. Lehman, Leen Decin, Dwayne E. Heard
Physical Chemistry Chemical Physics, 2023
Investigating Anomalous Photochemistry in the Inner Wind of IRC+10216 through Interferometric Observations of HC3N
Mark A. Siebert, Marie Van de Sande, Thomas J. Millar, Anthony J. Remijan
Astrophysical Journal, 2022
ATOMIUM: ALMA tracing the origins of molecules in dust forming oxygen rich M-type stars: Motivation, sample, calibration, and initial results
C. A. Gottlieb, L. Decin, A. M. S. Richards, F. De Ceuster, W. Homan, S. H. J. Wallström, T. Danilovich, T. J. Millar, M. Montargès, K. T. Wong, I. McDonald, A. Baudry, J. Bolte, E. Cannon, E. De Beck, A. de Koter, I. El Mellah, S. Etoka, D. Gobrecht, M. Gray, F. Herpin, M. Jeste, P. Kervella, T. Khouri, E. Lagadec, S. Maes, J. Malfait, K. M. Menten, H. S. P. Müller, B. Pimpanuwat, J. M. C. Plane, R. Sahai, M. Van de Sande, L. B. F. M. Waters, J. Yates, A. Zijlstra
Astronomy and Astrophysics, 2022
The impact of stellar companion UV photons on the chemistry of the circumstellar environments of AGB stars
M Van de Sande, T J Millar
Monthly Notices of the Royal Astronomical Society, 2022
The impact of UV photons from a stellar companion on the chemistry of AGB outflows
M. Van de Sande, T. J. Millar
Proceedings of the International Astronomical Union, 2022
The distribution of carbonaceous molecules and SiN around the S-type AGB star W Aquilae
T. Danilovich, M. Van de Sande, A. M. S. Richards, and
Proceedings of the International Astronomical Union, 2022
Chemistry on hot astrochemical dust surfaces: Sulfur in AGB outflows
Amy Wolstenholme-Hogg, Alexander D. James, John M. C. Plane, Marie Van de Sande
Proceedings of the International Astronomical Union, 2022
ATOMIUM: Halide molecules around the S-type AGB star W Aquilae
T. Danilovich, M. Van de Sande, J. M. C. Plane, T. J. Millar, P. Royer, M. A. Amor, K. Hammami, L. Decock, C. A. Gottlieb, L. Decin, A. M. S. Richards, E. De Beck, A. Baudry, J. Bolte, E. Cannon, F. De Ceuster, A. de Koter, S. Etoka, D. Gobrecht, M. Gray, F. Herpin, W. Homan, M. Jeste, P. Kervella, T. Khouri, E. Lagadec, S. Maes, J. Malfait, I. McDonald, K. M. Menten, M. Montargès, H. S. P. Müller, B. Pimpanuwat, R. Sahai, S. H. J. Wallström, L. B. F. M. Waters, K. T. Wong, J. Yates, A. Zijlstra
Astronomy and Astrophysics, 2021
ATOMIUM: The astounding complexity of the near circumstellar environment of the M-type AGB star R Hydrae: I. Morpho-kinematical interpretation of CO and SiO emission
W. Homan, B. Pimpanuwat, T. Danilovich, I. McDonald, S. H. J. Wallstrom, A. de Koter, A. M. S. Richards, A. Baudry, R. Sahai, T. J. Millar, et al
Astronomy and Astrophysics, 2021
Chemical modelling of dust-gas chemistry within AGB outflows-III. Photoprocessing of the ice and return to the ISM
M Van de Sande, C Walsh, T J Millar
Monthly Notices of the Royal Astronomical Society, 2021
Atomium: A high-resolution view on the highly asymmetric wind of the AGB star π1Gruis I. First detection of a new companion and its effect on the inner wind
Ward Homan, Miguel Montargès, Bannawit Pimpanuwat, Anita M. S. Richards, Sofia H. J. Wallström, Pierre Kervella, Leen Decin, Albert Zijlstra, Taissa Danilovich, Alex de Koter, Karl Menten, Raghvendra Sahai, John Plane, Kelvin Lee, Rens Waters, Alain Baudry, Ka Tat Wong, Tom J. Millar, Marie Van de Sande, Eric Lagadec, David Gobrecht, Jeremy Yates, Daniel Price, Emily Cannon, Jan Bolte, Frederik De Ceuster, Fabrice Herpin, Joe Nuth, Jan Philip Sindel, Dylan Kee, Malcolm D. Grey, Sandra Etoka, Manali Jeste, Carl A. Gottlieb, Elaine Gottlieb, Iain McDonald, Ileyk El Mellah, Holger S. P. Müller
Astronomy and Astrophysics, 2020
(Sub)stellar companions shape the winds of evolved stars
L. Decin, M. Montargès, A. M. S. Richards, C. A. Gottlieb, W. Homan, I. McDonald, I. El Mellah, T. Danilovich, S. H. J. Wallström, A. Zijlstra, A. Baudry, J. Bolte, E. Cannon, E. De Beck, F. De Ceuster, A. de Koter, J. De Ridder, S. Etoka, D. Gobrecht, M. Gray, F. Herpin, M. Jeste, E. Lagadec, P. Kervella, T. Khouri, K. Menten, T. J. Millar, H. S. P. Müller, J. M. C. Plane, R. Sahai, H. Sana, M. Van de Sande, L. B. F. M. Waters, K. T. Wong, J. Yates
Science, 2020
Chemical modelling of dust–gas chemistry within AGB outflows – II. Effect of the dust-grain size distribution
M Van de Sande, C Walsh, T Danilovich
Monthly Notices of the Royal Astronomical Society, 2020
An ALMA view of SO and SO2 around oxygen-rich AGB stars
T Danilovich, A M S Richards, L Decin, M Van de Sande, C A Gottlieb
Monthly Notices of the Royal Astronomical Society, 2020
Erratum: Determining the effects of clumping and porosity on the chemistry in a non-uniform AGB outflow (Astronomy and Astrophysics (2018) 616 (A106) DOI: 10.1051/0004-6361/201732276)
M. Van de Sande, J. O. Sundqvist, T. J. Millar, D. Keller, W. Homan, A. de Koter, L. Decin, F. De Ceuster
Astronomy and Astrophysics, 2020
AGB outflows as tests of chemical kinetics and radiative transfer models
M. Van de Sande, T. Danilovich, L. Decin
Proceedings of the International Astronomical Union, 2020
Chemical modelling of dust-gas chemistry within AGB outflows - I. Effect on the gas-phase chemistry
M Van de Sande, C Walsh, T P Mangan, L Decin
Monthly Notices of the Royal Astronomical Society, 2019
Measurements of Low Temperature Rate Coefficients for the Reaction of CH with CH2O and Application to Dark Cloud and AGB Stellar Wind Models
Niclas A. West, Tom J. Millar, Marie Van de Sande, Edward Rutter, Mark A. Blitz, Leen Decin, Dwayne E. Heard
Astrophysical Journal, 2019
Reduction of the maximum mass-loss rate of OH/IR stars due to unnoticed binary interaction
L. Decin, W. Homan, T. Danilovich, A. de Koter, D. Engels, L. B. F. M. Waters, S. Muller, C. Gielen, D. A. García-Hernández, R. J. Stancliffe, M. Van de Sande, G. Molenberghs, F. Kerschbaum, A. A. Zijlstra, I. El Mellah
Nature Astronomy, 2019
Author Correction: Reduction of the maximum mass-loss rate of OH/IR stars due to unnoticed binary interaction (Nature Astronomy, (2019), 3, 5, (408-415), 10.1038/s41550-019-0703-5)
L. Decin, W. Homan, T. Danilovich, A. de Koter, D. Engels, L. B. F. M. Waters, S. Muller, C. Gielen, D. A. García-Hernández, R. J. Stancliffe, M. Van de Sande, G. Molenberghs, F. Kerschbaum, A. A. Zijlstra, I. El Mellah
Nature Astronomy, 2019
An ALMA view of CS and SiS around oxygen-rich AGB stars
T Danilovich, A M S Richards, A I Karakas, M Van de Sande, L Decin, F De Ceuster
Monthly Notices of the Royal Astronomical Society, 2019
The Role of Internal Photons on the Chemistry of the Circumstellar Envelopes of AGB Stars
M. Van de Sande, T. J. Millar
Astrophysical Journal, 2019
ALMA spectrum of the extreme OH/IR star OH 26.5+0.6
K. Justtanont, S. Muller, M. J. Barlow, D. Engels, D. A. García-Hernández, M. A. T. Groenewegen, M. Matsuura, H. Olofsson, D. Teyssier, I. Marti-Vidal, T. Khouri, M. Van de Sande, W. Homan, T. Danilovich, A. de Koter, L. Decin, L. B. F. M. Waters, R. Stancliffe, W. Vlemmings, P. Royer, F. Kerschbaum, C. Paladini, J. Blommaert, R. de Nutte
Proceedings of the International Astronomical Union, 2019
The chemistry in clumpy AGB outflows
M. Van de Sande, J. O. Sundqvist, T. J. Millar, D. Keller, L. Decin
Proceedings of the International Astronomical Union, 2018
Molecular data needs for modelling AGB stellar winds and other molecular environments
Taïssa Danilovich, Leen Decin, Marie Van de Sande
Galaxies, 2018
ALMA detection of a tentative nearly edge-on rotating disk around the nearby AGB star R Doradus
Ward Homan, Taissa Danilovich, Leen Decin, Alex de Koter, Joseph Nuth, Marie Van de Sande
Astronomy and Astrophysics, 2018
Determining the effects of clumping and porosity on the chemistry in a non-uniform AGB outflow
M. Van de Sande, J. O. Sundqvist, T. J. Millar, D. Keller, W. Homan, A. de Koter, L. Decin, F. De Ceuster
Astronomy and Astrophysics, 2018
Chemical content of the circumstellar envelope of the oxygen-rich AGB star R Doradus: Non-LTE abundance analysis of CO, SiO, and HCN
M. Van de Sande, L. Decin, R. Lombaert, T. Khouri, A. de Koter, F. Wyrowski, R. De Nutte, W. Homan
Astronomy and Astrophysics, 2018
Study of the aluminium content in AGB winds using ALMA: Indications for the presence of gas-phase (Al 2 O 3) clusters
L. Decin, A. M. S. Richards, L. B. F. M. Waters, T. Danilovich, D. Gobrecht, T. Khouri, W. Homan, J. M. Bakker, M. Van de Sande, J. A. Nuth, E. De Beck
Astronomy and Astrophysics, 2017
Sulphur-bearing molecules in AGB stars: I. The occurrence of hydrogen sulphide
T. Danilovich, M. Van de Sande, E. De Beck, L. Decin, H. Olofsson, S. Ramstedt, T. J. Millar
Astronomy and Astrophysics, 2017
Search for exoplanets around pulsating stars of A–F type in Kepler short-cadence data and the case of KIC 8197761
Paulina Sowicka, Gerald Handler, Bartłomiej Dębski, David Jones, Marie Van de Sande, Péter I. Pápics
Monthly Notices of the Royal Astronomical Society, 2017
Nucleosynthesis in AGB stars traced by oxygen isotopic ratios: I. Determining the stellar initial mass by means of the 17O/18O ratio
R. De Nutte, L. Decin, H. Olofsson, R. Lombaert, A. de Koter, A. Karakas, S. Milam, S. Ramstedt, R. J. Stancliffe, W. Homan, M. Van de Sande
Astronomy and Astrophysics, 2017
Signatures of internal rotation discovered in the Kepler data of five slowly pulsating B stars
P. I. Pápics, A. Tkachenko, T. Van Reeth, C. Aerts, E. Moravveji, M. Van de Sande, K. De Smedt, S. Bloemen, J. Southworth, J. Debosscher, E. Niemczura, J. F. Gameiro
Astronomy and Astrophysics, 2017
Determining the effect of a non-uniform AGB outflow on its chemistry
M. Van de Sande, J. O. Sundqvist, T. J. Millar, L. Decin
Proceedings of the International Astronomical Union, 2017
ALMA-resolved salt emission traces the chemical footprint and inner wind morphology of VY Canis Majoris
L. Decin, A. M. S. Richards, T. J. Millar, A. Baudry, E. De Beck, W. Homan, N. Smith, M. Van de Sande, C. Walsh
Astronomy and Astrophysics, 2016
Unraveling the Dust Formation Process in R Dor
M. Van de Sande, L. Decin, R. Lombaert, C. Walsh, T. Khouri, X. Li, T.J. Millar
Eas Publications Series, 2015
The rms-flux relation in accreting white dwarfs: Another nova-like variable and the first dwarf nova
M. Van de Sande, S. Scaringi, C. Knigge
Monthly Notices of the Royal Astronomical Society, 2015

Marie Van de Sande

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