Article
Astronomy & Astrophysics
P. J. Rodenkirch, T. Rometsch, C. P. Dullemond, P. Weber, W. Kley
Summary: The study investigates the physical mechanisms behind the formation of the crescent-shaped asymmetry and ring structures in the HD 163296 disk, suggesting that they may be attributed to planet-disk interactions. Simulation results show that the crescent-shaped feature can be qualitatively modeled, and provide insights by constraining the level of viscosity and planetary mass.
ASTRONOMY & ASTROPHYSICS
(2021)
Article
Astronomy & Astrophysics
J. A. Sturm, M. K. Mcclure, C. J. Law, D. Harsono, J. B. Bergner, E. Dartois, M. N. Drozdovskaya, S. Ioppolo, K. I. Oberg, M. E. Palumbo, Y. J. Pendleton, W. R. M. Rocha, H. Terada, R. G. Urso
Summary: Observations of edge-on disks play an important role in understanding protoplanetary disk properties. However, current models struggle to reproduce both the spectral energy distributions and scattered light observations due to differences in geometry and dust properties at different wavelengths. In this study, the authors successfully constrained the geometry and characteristics of the protoplanetary disk HH 48 NE using a parameterized dust model and a Monte Carlo framework. The findings provide insights into the physical structure and icy chemistry of this disk.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
J. A. Sturm, M. K. Mcclure, J. B. Bergner, D. Harsono, E. Dartois, M. N. Drozdovskaya, S. Ioppolo, K. I. Oberg, C. J. Law, M. E. Palumbo, Y. J. Pendleton, W. R. M. Rocha, H. Terada, R. G. Urso
Summary: This study models the ice absorption features in protoplanetary disks to determine the abundance of the main ice species in the disk. The results show that the uncertainty of the physical parameters can affect the determination of ice abundance.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
P. Curone, A. F. Izquierdo, L. Testi, G. Lodato, S. Facchini, A. Natta, P. Pinilla, N. T. Kurtovic, C. Toci, M. Benisty, M. Tazzari, F. Borsa, M. Lombardi, C. F. Manara, E. Sanchis, L. Ricci
Summary: Researchers have discovered clues to the existence of a massive planet around a VLM star based on high-resolution observations from ALMA. They used simulations to replicate the morphology and location of the observed dust ring, estimating a minimum planet mass of about 1.4 M-Jup at a distance of 9-10 au. This finding challenges our understanding of planet formation around VLM stars.
ASTRONOMY & ASTROPHYSICS
(2022)
Article
Astronomy & Astrophysics
C. Bergez-Casalou, B. Bitsch, N. T. Kurtovic, P. Pinilla
Summary: New ALMA observations provide constraints on planet formation in protoplanetary disks. By using simulations and observations, it is found that giant planets perturb the radial gas velocities of the disk and create traffic jams in the dust. High-resolution observations are needed to distinguish important features in the inner part of the disk. The study also shows the potential of ALMA to constrain different stages of planet formation.
ASTRONOMY & ASTROPHYSICS
(2022)
Article
Astronomy & Astrophysics
M. Villenave, K. R. Stapelfeldt, G. Duchene, F. Menard, M. Lambrechts, A. Sierra, C. Flores, W. R. F. Dent, S. Wolff, A. Ribas, M. Benisty, N. Cuello, C. Pinte
Summary: This study investigates the mechanism of dust concentration in a protoplanetary disk through observations and modeling, finding that the thin dust scale height is favorable for planetary growth by pebble accretion, providing theoretical support for the efficient settling of large grains in the disk.
ASTROPHYSICAL JOURNAL
(2022)
Article
Astronomy & Astrophysics
Anina Timmermann, Yutong Shan, Ansgar Reiners, Andreas Pack
Summary: Equilibrium condensation simulations provide insights into the composition of exoplanets and their relation to their host star. In this study, a simplified model was developed to simulate condensation in protoplanetary disks, investigating the formation characteristics of rocky planets and the bulk compositions of planets around chemically diverse stars by varying pressure and elemental abundance pattern.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
A. Kessler, Y. Alibert
Summary: In the core accretion scenario of planet formation, the accretion of millimetre- to centimetre-sized pebbles allows for rapid core growth within the disk lifetime, while the accretion of kilometre-sized planetesimals often results in longer planet formation timescales. This study investigates the interplay between the two accretion processes in a disk containing both pebbles and planetesimals, and concludes that the late accretion of planetesimals is a critical factor in the giant planet formation process in hybrid pebble-planetesimal scenarios.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Alex J. Cridland, Giovanni P. Rosotti, Benoit Tabone, Lukasz Tychoniec, Melissa McClure, Pooneh Nazari, Ewine F. van Dishoeck
Summary: Recent surveys have questioned whether the first steps of planet formation occur in younger systems with enough dust in their embedded disks. This study models the collapse of a dusty proto-stellar cloud and finds that moderately coupled dust grains with a dust-to-gas mass ratio near unity can drive the streaming instability for planetesimal formation. The results suggest that planetesimal formation occurs earlier in the lifetime of young stars and can build the core of the first giant planet.
ASTRONOMY & ASTROPHYSICS
(2022)
Article
Astronomy & Astrophysics
P. Pinilla, N. T. Kurtovic, M. Benisty, C. F. Manara, A. Natta, E. Sanchis, M. Tazzari, S. M. Stammler, L. Ricci, L. Testi
Summary: The frequency of Earth-sized planets in habitable zones appears to be higher around M-dwarfs, making these systems exciting laboratories to investigate planet formation. Observations of protoplanetary disks around very low-mass stars and brown dwarfs remain challenging and little is known about their properties. The characteristics of the disk around CIDA 1 challenge current dust evolution models, particularly processes like fragmentation, growth, and diffusion of particles inside pressure bumps.
ASTRONOMY & ASTROPHYSICS
(2021)
Article
Astronomy & Astrophysics
M. Oosterloo, I. Kamp, W. van Westrenen, C. Dominik
Summary: The abundance of CHNOS in planetesimals and planets is crucial for understanding their initial composition. In this study, we compared the timescales of various processes in planet-forming disks to determine the regions where these processes are fully coupled. We developed the SHAMPOO code to track the CHNOS abundances in dust particles and investigated the effects of fragmentation velocity and home aggregate filling factor on the amount of CHNOS-bearing ices.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
N. Oberg, S. Cazaux, I. Kamp, T. -M. Brundl, W. F. Thi, C. Immerzeel
Summary: This study aims to explore the process of ice formation in CPDs to determine which disk properties are consistent with the formation of an icy moon system. By analyzing the radiation thermochemical code ProDiMo, we have derived the radial ice abundance and rate of ice formation in a model CPDs. The results show that three-body reactions play an important role in water formation and the CPD must have a depleted dust midplane to produce ice-rich satellites.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Nicolas Kaufmann, Yann Alibert
Summary: The effects of planetesimal fragmentation on planet formation were investigated using a population synthesis approach. The study found that fragmentation can either enhance or hinder planet formation, depending on the size of solids generated in collisions. Larger fragments promote accretion beyond the ice line, while smaller fragments hinder the formation process due to shorter drift timescales.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Christian Eistrup, L. Ilsedore Cleeves, Sebastiaan Krijt
Summary: This study aims to model the compositional evolution of volatile ices on grains of different sizes, considering time-dependent grain growth and multiple constant grain sizes. The results show that grain growth reduces the available grain-surface area for ice-phase reactions, leading to a decrease in reaction efficiency. Larger grain sizes have a smaller impact on the change in C/O ratio in the gas phase. Choosing a constant grain size from a grain evolution model may be an appropriate simplification when studying the impact of grain growth on chemical evolution.
ASTRONOMY & ASTROPHYSICS
(2022)
Article
Astronomy & Astrophysics
N. T. Kurtovic, P. Pinilla, Anna B. T. Penzlin, M. Benisty, L. Perez, C. Ginski, A. Isella, W. Kley, F. Menard, S. Perez, A. Bayo
Summary: By analyzing the observations and simulations of CS Cha, the study suggests a high possibility of planetary formation in circumbinary orbits, and the combination of low eccentricity and axisymmetry provides further evidence for this hypothesis.
ASTRONOMY & ASTROPHYSICS
(2022)
Article
Astronomy & Astrophysics
Claudia Toci, Giuseppe Lodato, Francesco Gerardo Livio, Giovanni Rosotti, Leon Trapman
Summary: A robust knowledge of the observed disc radius using gas tracers such as (CO)-C-12 is pivotal to understand the mechanism responsible for accretion in protoplanetary discs. This letter presents an analytical solution for the evolution of disc radii in viscously evolving protoplanetary discs using (CO)-C-12 as a tracer, assuming that the (CO)-C-12 radius is the radius where the surface density of the disc is equal to the threshold for CO photodissociation. Our results suggest that freeze-out also plays an important role in setting the disc size, in addition to photodissociation.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)
Article
Astronomy & Astrophysics
P. Nazari, B. Tabone, G. P. Rosotti
Summary: This study investigates the lack of methanol emission from some massive protostellar systems. It finds that the presence of a disk does not significantly affect the temperature structure and methanol emission from high-mass protostars. The methanol emission is lower for models with high millimeter opacity dust, but a large disk is needed for this effect to be effective. The low methanol emission in high-luminosity sources can be explained by the presence of HII regions without methanol.
ASTRONOMY & ASTROPHYSICS
(2023)
Review
Astronomy & Astrophysics
Karin I. Oberg, Stefano Facchini, Dana E. Anderson
Summary: Planets form in disks of gas and dust around young stars. The chemical composition of these disks, particularly the volatile elements, is determined by both inheritance and in situ chemistry. The links between disk chemistry, structure, and dynamics offer unique insights into planet formation, but also pose challenges for modeling. Understanding disk chemistry is important for studying the evolution of disks and the composition of mature planets.
ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Alex J. Cridland, Stefano Facchini, Ewine F. van Dishoeck, Myriam Benisty
Summary: By studying the physical and chemical models of the 5 Myr old PDS 70 system, a volatile carbon-to-oxygen number ratio above unity was found in the outer disk. This was used to estimate the atmospheric C/O ratio of the planets PDS 70b and PDS 70c. The research provides a foundation for understanding the disk and planet formation scenario in the PDS 70 system.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Yapeng Zhang, Christian Ginski, Jane Huang, Alice Zurlo, Herve Beust, Jaehan Bae, Myriam Benisty, Antonio Garufi, Michiel R. R. Hogerheijde, Rob G. G. van Holstein, Matthew Kenworthy, Maud Langlois, Carlo F. F. Manara, Paola Pinilla, Christian Rab, Alvaro Ribas, Giovanni P. P. Rosotti, Jonathan Williams
Summary: In this study, we investigated and compared circumstellar disks in three stellar multiple systems using near-infrared scattered-light imaging. Our observations revealed that the presence of companion stars affects the morphology and evolution of the disks, potentially resulting in different planetary populations. The comparison of the three systems showed that the influence of stellar companions on disk structures decreases with increasing separation.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Francesco Zagaria, Stefano Facchini, Anna Miotello, Carlo F. F. Manara, Claudia Toci, Cathie J. J. Clarke
Summary: The Atacama Large Millimeter/submillimeter Array (ALMA) has not yet provided definitive answers on the disc evolution mechanisms. An alternative method based on (CO)-C-12 fluxes has been introduced to study disc evolution, which can be easily collected using lower resolution observations. The new method has been tested and compared with data, showing good agreement when considering CO depletion.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Eleonora Fiorellino, Lukasz Tychoniec, Fernando Cruz-Saenz de Miera, Simone Antoniucci, Agnes Kospal, Carlo F. Manara, Brunella Nisini, Giovanni Rosotti
Summary: This work aims to fill the gap in the poorly constrained information about the accretion luminosity and stellar parameters for the youngest sources. Using a self-consistent method, we calculated the accretion and stellar properties for 50 young stars for the first time. Our analysis focused on 39 confirmed protostars and found that their mass accretion rates range between 10(-8) and 10(-4) solar masses per year. We found systematically larger mass accretion rates for the Class I sample compared to Class II objects.
ASTROPHYSICAL JOURNAL
(2023)
Article
Astronomy & Astrophysics
Yinhao Wu, Yi-Xian Chen, Haochang Jiang, Ruobing Dong, Enrique Macias, Min-Kai Lin, Giovanni P. Rosotti, Vardan Elbakyan
Summary: A novel approach to distinguishing wind-driven and turbulence-driven accretion has been proposed by studying the gap and ring morphology of planet-forming discs in ALMA continuum. Results from hydrodynamical simulations show that gap-opening planets in wind-driven accreting discs generate characteristic dust substructures that differ from those in purely viscous discs. The classification of planet-induced features sets up a potential method to constrain the strength of magnetized disc wind and viscosity based on observed morphology.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)
Article
Astronomy & Astrophysics
P. Curone, L. Testi, E. Macias, M. Tazzari, S. Facchini, J. P. Williams, C. J. Clarke, A. Natta, G. Rosotti, C. Toci, G. Lodato
Summary: Observations of protoplanetary disks require a multiwavelength approach to fully understand their physical mechanisms and planet formation. This study focuses on CX Tau, using observations and analysis from multiple telescopes and wavelengths. The results show consistent findings with theoretical predictions and peculiar behavior in the centimeter wavelength observations.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
O. Balsalobre-Ruza, I. de Gregorio-Monsalvo, J. Lillo-Box, N. Huelamo, A. Ribas, M. Benisty, J. Bae, S. Facchini, R. Teague
Summary: By reanalyzing the ALMA observations of PDS 70, researchers have found tentative evidence of the formation of exotrojan bodies in the co-orbital Lagrangian regions L-4/L-5. However, further observations are needed to confirm this discovery.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Perez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Summary: PDS 70 is the only young disk where multiple planets have been detected by direct imaging. Observations of the disk reveal a large cavity and the presence of wind features associated with oxygen and helium, which is unusual for low accretors.
ASTROPHYSICAL JOURNAL
(2023)
Article
Astronomy & Astrophysics
Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoit Tabone, Carlo F. Manara, Marco Tazzari
Summary: As the classic viscous paradigm for protoplanetary disk accretion is challenged by observational evidence, the alternative scenario of MHD disk winds is being explored. This study presents a method to distinguish between viscous and MHD models based on the evolution of disk mass-accretion rate distribution in a disk population. Analytical calculations and numerical simulations show that the spread of this distribution decreases over time, with a less pronounced effect in MHD-dominated populations compared to viscous populations. The difference between the two models can be detected using current observational facilities.
ASTROPHYSICAL JOURNAL LETTERS
(2023)
Article
Astronomy & Astrophysics
Richard Alexander, Giovanni Rosotti, Philip J. Armitage, Gregory J. Herczeg, Carlo F. Manara, Benoit Tabone
Summary: We find that the distribution of observed accretion rates is a powerful tool to distinguish between two mechanisms of disc accretion, namely turbulent transport of angular momentum and magnetized disc winds. A sample of 300 observed accretion rates would be sufficient to confidently differentiate between the two mechanisms, even with conservative assumptions. Current observations of T Tauri star accretion rates are too small and heterogeneous to provide a clear answer, making both viscous and wind-driven models valid.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)