Article
Astronomy & Astrophysics
E. Miller, S. Marino, S. M. Stammler, P. Pinilla, C. Lenz, T. Birnstiel, Th Henning
Summary: Studying the determinants of exoKuiper belt width is complex, as observations have shown a nearly fourfold increase in width in mature systems compared to narrow belts in protoplanetary discs. Research suggests that dust traps during migration may facilitate planetesimal formation, leading to a positive correlation between inward radial speed and final planetesimal belt width.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2021)
Article
Astronomy & Astrophysics
Hossam Aly, Jean-Francois Gonzalez, Rebecca Nealon, Cristiano Longarini, Giuseppe Lodato, Daniel J. Price
Summary: Gas and dust in inclined orbits around binaries experience precession induced by binary gravitational torque, leading to density enhancements called "dust traffic jams" where weakly coupled dust alters radial drift. These traffic jams exist at different disc inclinations and binary eccentricities, providing significant dust density enhancements and playing a crucial role in the evolution of dust disc angular momentum.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2021)
Article
Astronomy & Astrophysics
Alice Somigliana, Claudia Toci, Giovanni Rosotti, Giuseppe Lodato, Marco Tazzari, Carlo F. Manara, Leonardo Testi, Federico Lepri
Summary: Large surveys of star-forming regions have revealed power-law correlations between stellar mass and disc parameters, but the reasons behind these correlations and their evolution are uncertain. This study conducts a theoretical analysis and numerical simulations to investigate the impact of viscous evolution on these correlations. The results show that viscous evolution enforces the correlations to have the same slope, and the increasing trend observed is a consequence of a positive correlation between viscous time-scale and stellar mass. Comparisons with observational data help constrain the parameter space of the initial conditions.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Samuel M. Karlin, Olja Panic, Sven van Loo
Summary: The major satellites of Jupiter and Saturn are believed to have formed in circumplanetary discs (CPDs), which orbit forming giant protoplanets. Gas and dust in CPDs have different distributions and affect each other by drag, which varies with grain size. Simulations of multiple dust grain sizes with separate dynamics have not been done before. The amount of dust of each grain size in CPDs was assessed through multifluid 3D hydrodynamical simulations, showing a truncated MRN distribution at smaller grain sizes and very inefficient accretion of large dust grains to CPDs due to dust filtration. The dust masses in CPDs are small, with a mass ratio similar to a few x 10(-6) to the protoplanet, in line with observed CPD fluxes.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)
Article
Astronomy & Astrophysics
Ian Rabago, Zhaohuan Zhu, Rebecca G. Martin, Stephen H. Lubow
Summary: We present the first grid-based simulations of the polar alignment of a circumbinary disc. By using the grid-based code athena++, we investigate the evolution of an inclined disc around an eccentric binary. Our results show that high viscosity leads to polar alignment, while low viscosity results in little alignment over 1000 binary orbital periods. We also observe anticyclonic vortices at the inner edge of the disc at very low viscosities, which can have significant implications for the evolution of circumbinary systems.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)
Article
Astronomy & Astrophysics
Benoit Tabone, Giovanni P. Rosotti, Alexander J. Cridland, Philip J. Armitage, Giuseppe Lodato
Summary: The evolution of protoplanetary discs and planet formation is influenced by angular momentum transport and mass-loss processes. The paradigm of viscosity has been challenged in recent years, with MHD disc winds emerging as a new scenario for disc accretion.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Gavin A. L. Coleman
Summary: Planet formation models often skip the crucial step of planetesimal/proto-embryo formation. This study includes prescriptions for planetesimal and proto-embryo formation from trapped pebbles in pressure bumps, examining their sizes and distributions throughout the disc. Results show that planetesimal sizes increase with orbital distance and proto-embryo masses increase with orbital radius. By combining different accretion scenarios, more massive proto-embryos can form at larger distances, allowing for a better understanding of planetary system formation.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2021)
Article
Astronomy & Astrophysics
M. Fritscher, J. Teiser
Summary: The stability of planetesimals is crucial for their growth and evolution, and it depends on the stability, adhesion, and fragmentation of macroscopic agglomerates. In this study, we investigate the stability of highly porous CO2 agglomerates, which are abundant in the outer parts of protoplanetary discs. Our experiments show that the tensile strength of the agglomerates follows a power law dependence on the volume filling. The surface energy of the agglomerates is calculated to be γ = 0.060 +/- 0.022 J m(-2).
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Matthew Alessi, Ralph E. Pudritz
Summary: Recent surveys have found that protoplanetary discs have lower levels of turbulence than expected, and magnetized disc winds may play a dominant role in angular momentum transport. This has important implications for the process of planet formation. By computing the physical and chemical evolution of discs and the formation and migration of planets, researchers have found that populations produced from discs with different levels of turbulence and winds strength fit better with observations, compared to populations with constant values. These models suggest a substantial population of super Earths at specific orbital radii, as well as distinct populations of hot Jupiter and warm Jupiter planets.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Thomas J. Haworth, Jinyoung S. Kim, Lin Qiao, Andrew J. Winter, Jonathan P. Williams, Cathie J. Clarke, James E. Owen, Stefano Facchini, Megan Ansdell, Mikhel Kama, Giulia Ballabio
Summary: We searched for C I 1-0 emission towards eight proplyds in NGC 1977 using the APEX telescope, but no detections were made despite reaching sensitivities deeper than previous observations. Comparison with external photo-evaporation simulations suggests that the non-detections are consistent with very low mass proplyd discs.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Ayaka Okuya, Shigeru Ida, Ryuki Hyodo, Satoshi Okuzumi
Summary: A growing number of debris discs around metal-polluted white dwarfs have been detected. They are believed to originate from tidally disrupted exoplanetary bodies and contribute to the accretion of metals onto the white dwarfs. Previous studies proposed that the high accretion rates and the presence of rocky materials in the photosphere can be explained by the runaway accretion of silicate particles due to gas drag. However, this study shows that if re-condensation is taken into account, runaway accretion does not occur and the accretion rate is limited. Alternatively, the presence of volatile gas, such as water vapor, enhances the silicate accretion rate through gas drag and can explain the observed refractory-rich accretion.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)
Article
Astronomy & Astrophysics
J. Humphries, C. Hall, T. J. Haworth, S. Nayakshin
Summary: This paper discusses the detection of protoplanets born through gravitational instability (GI) and suggests that they may remain in a pre-collapse phase for up to 10^7 years after formation, with atmospheres too cold to emit in near-infrared or Hα, but possibly detectable through dust emission with ALMA. The study finds that detection in a disc at 140 pc would require a few hundred minutes of ALMA observation time, with protoplanets of 3-5 M_J having the highest chance of being detected. High-resolution surveys of young, massive, and face-on discs are proposed as offering the best chance for observing protoplanets and potentially placing constraints on the protoplanet mass spectrum and prevalence of GI as a planet formation mechanism.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2021)
Article
Astronomy & Astrophysics
Leandro Esteves, Andra Izidoro, Bertram Bitsch, Seth A. Jacobson, Sean N. Raymond, Rogerio Deienno, Othon C. Winter
Summary: The study suggests that perfect accretion is a suitable approximation for dynamic purposes in the scenario described. Despite common fragmentation events, only around 10% of the system mass is fragmented during a typical 'late instability phase', with most fragments being reacreted by surviving planets. The limited total mass in fragments proves insufficient to qualitatively alter the final system dynamical configuration compared to simulations where fragmentation is disregarded.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Maxwell X. Cai, Jonathan C. Tan, Simon Portegies Zwart
Summary: This study investigates the formation process of planetesimals in the theory of Inside-Out Planet Formation (IOPF) through collisional evolution simulations. The research finds that the planetesimal ring undergoes oligarchic evolution, resulting in 2 or 3 surviving oligarchs on nearly coplanar and circular orbits. However, a relatively massive secondary planet always remains, which is inconsistent with the observed properties of innermost planet pairs.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2022)
Article
Astronomy & Astrophysics
Rixin Li, Yi-Xian Chen, Douglas N. C. Lin
Summary: Our study proposes a promising formation mechanism for super-Earths by examining dust trapping in pressure bumps induced by magnetospheric truncation. We find that efficient dust growth and accumulation are possible in less turbulent discs, providing a solid foundation for further growth towards planetesimals and planetary embryos. Additionally, different dominant processes result in different ways of forming planetesimals and these diverse dust behaviors help explain observed phenomena in protoplanetary discs.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(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)
Article
Astronomy & Astrophysics
A. F. Izquierdo, L. Testi, S. Facchini, G. P. Rosotti, E. F. van Dishoeck, L. Wolfer, T. Paneque-Carreno
Summary: The study aims to devise an automated and statistically robust technique to detect and quantify kinematical perturbations caused by planets in a gas disc, and accurately infer the location of the planets. The authors conducted hydrodynamical simulations and radiative transfer calculations to analyze the gas kinematics in discs and successfully detected the presence and location of embedded planets.
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
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
Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Andrea Banzatti, Giovanni Rosotti, Gijs D. Mulders, Michiel Lambrechts, Feng Long, Gregory J. Herczeg
Summary: Substructures in protoplanetary disks, such as gaps, can trap dust particles and affect the distribution of pebbles in the disk. These gaps can impact the delivery of pebbles, which is important for the formation of inner planets. They can also affect the distribution of volatiles, like water vapor, within the disk. In this study, we investigate the influence of gaps in the outer gas disk on water vapor enrichment in the inner disk using a disk evolution model. We find that the abundance of water vapor in the inner disk is strongly influenced by the fragmentation velocity and turbulence, which determine the intensity and duration of pebble delivery and enrichment in the disk.
ASTROPHYSICAL JOURNAL
(2023)
Article
Astronomy & Astrophysics
Leon Trapman, Giovanni Rosotti, Ke Zhang, Benoit Tabone
Summary: The mechanism driving the evolution of protoplanetary disks is still uncertain, and the direct detection of turbulence or disk winds has been difficult. To differentiate between these mechanisms, the evolution of the disk size is studied. The relation between the observed gas disk size and the physical disk size is examined, and a correlation between gas column density and disk mass is found. The decrease in disk size in the older Upper Sco region may be due to significant external photoevaporation.
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)
Article
Astronomy & Astrophysics
Elia Pizzati, Giovanni P. Rosotti, Benoit Tabone
Summary: This study assesses the strength of gas turbulence in protoplanetary discs by measuring the vertical distribution of dust component in six discs observed in the DSHARP programme. By observing the differences in gap contrasts along the major and minor axes, a radiative transfer model is used to replicate these features for different dust scale heights. The findings suggest that lower scale heights provide better agreement with the data, indicating low turbulence levels of alpha(SS) less than or similar to 10(-3) - 10(-4). For other systems considered, no significant constraints on the disc vertical structure were obtained, likely due to low disc inclination or insufficiently deep gaps. An empirical criterion is provided to evaluate the suitability of a given disc for measuring the vertical scale height.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
(2023)