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
J. A. Sturm, M. K. McClure, D. Harsono, S. Facchini, F. Long, M. Kama, E. A. Bergin, E. F. van Dishoeck
Summary: This study investigates the measurements of the carbon-to-hydrogen ratio in protoplanetary disks and explores the mechanisms and evolutionary trends of gaseous carbon depletion. By using models and analyzing observational data, the study determines the magnitude of carbon depletion and the effects of disk material drift and dust structure.
ASTRONOMY & ASTROPHYSICS
(2022)
Article
Astronomy & Astrophysics
L. Cacciapuoti, E. Macias, A. J. Maury, C. J. Chandler, N. Sakai, L. Tychoniec, S. Viti, A. Natta, M. De Simone, A. Miotello, C. Codella, C. Ceccarelli, L. Podio, D. Fedele, D. Johnstone, Y. Shirley, B. J. Liu, E. Bianchi, Z. E. Zhang, J. Pineda, L. Loinard, F. Menard, U. Lebreuilly, R. S. Klessen, P. Hennebelle, S. Molinari, L. Testi, S. Yamamoto
Summary: Recent studies have suggested early dust grain growth in protostellar envelopes infalling on young disks, potentially impacting initial conditions of planet formation. This study aims to determine the maximum grain size in the envelope of the class 0/I protostar L1527 IRS using observational data from multiple wavelength bands. The results indicate a variation of dust properties in the envelope, potentially indicating in situ grain growth or differential collapse from the parent core.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Takahiro Ueda, Satoshi Okuzumi, Akimasa Kataoka, Mario Flock
Summary: We investigated the physical properties and midplane heating effects of the CW Tau disk using physical models and ALMA dust continuum observations. The results show that if the maximum dust size is less than or equal to 100 μm, the predicted brightness temperatures exceed the observations. Scattering by particles can reduce the observed brightness temperatures. The study also provides some constraints on the different levels of disk activity.
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
Felix Jungmann, Gerhard Wurm
Summary: This study explores the impact of charge exchange on particle aggregation during collisions, demonstrating that charging can induce the formation of particle aggregates. Experimental observations of submm grain motion following collisions revealed that particles can continue to adhere at high velocities, contrary to expectations based on surface forces, supporting the formation of aggregates as a crucial step in early planet formation beyond the traditional bouncing barrier.
ASTRONOMY & ASTROPHYSICS
(2021)
Article
Astronomy & Astrophysics
Shigeru Ida, Tristan Guillot, Ryuki Hyodo, Satoshi Okuzumi, Andrew N. Youdin
Summary: The study aims to understand and quantify the impact of the water snow line on the formation of rock-rich and ice-rich planetesimals, focusing on the formation of rock-rich planetesimals. The numerical results suggest that the runaway pile-up of silicate particles (formation of rocky planetesimals) occurs if the pebble-to-gas mass flux ratio is greater than or similar to [(alpha (Dz)/alpha (acc))/3 x 10(-2)](1/2).
ASTRONOMY & ASTROPHYSICS
(2021)
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
Masahiro Ogihara, Yasunori Hori, Masanobu Kunitomo, Kenji Kurosaki
Summary: The study demonstrates that the formation of giant planets with large metal masses can be explained by a mechanism involving envelope mass loss during giant impacts and core accretion during disk evolution. Gas accretion and photoevaporation are key factors in the formation of giant planets with large metal fractions.
ASTRONOMY & ASTROPHYSICS
(2021)
Article
Astronomy & Astrophysics
Feng Long, Arthur D. Bosman, Paolo Cazzoletti, Ewine F. van Dishoeck, Karin I. Oberg, Stefano Facchini, Marco Tazzari, Viviana V. Guzman, Leonardo Testi
Summary: The study investigates HNC and HCN line emission in protoplanetary disks using the DALI model, finding brighter line emission in models with larger disk flaring angles and higher UV fluxes. HNC and HCN are predicted to be abundant in the warm surface layer and outer midplane region, resulting in ring-shaped emission patterns. The HNC-to-HCN line intensity ratio increases with radius, affected by UV flux and C and O abundances.
ASTRONOMY & ASTROPHYSICS
(2021)
Article
Astronomy & Astrophysics
Anders Johansen, Caroline Dorn
Summary: The pathway to forming the iron-rich planet Mercury remains mysterious. However, this study found that in the hot inner regions of the protoplanetary disc, iron particles nucleate homogeneously due to their high surface tension, resulting in the formation of large iron pebbles, which explains the abundance of iron in Mercury.
ASTRONOMY & ASTROPHYSICS
(2022)
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
Bertram Bitsch, Sean N. Raymond, Lars A. Buchhave, Aaron Bello-Arufe, Alexander D. Rathcke, Aaron David Schneider
Summary: In the pebble accretion scenario, the position of growing planetary cores relative to the water ice line plays a key role in determining the water content of inner planets. Pebbles blocked outside the water ice line result in a dry inner disk, while those blocked inside release water vapor, leading to wetter inner planets.
ASTRONOMY & ASTROPHYSICS
(2021)
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
A. Gupta, A. Miotello, C. F. Manara, J. P. Williams, S. Facchini, G. Beccari, T. Birnstiel, C. Ginski, A. Hacar, M. Kueffmeier, L. Testi, L. Tychoniec, H. -W Yen
Summary: It is found that some Class II sources in close vicinity to a reflection nebula may be undergoing late infall of material onto the disk, which can significantly affect disk evolution and planet formation. Observations and analyses reveal the existence of large-scale gas structures and their association with reflection nebulae around Class II sources. These findings suggest that a considerable fraction of Class II disks in nearby star-forming regions may undergo late accretion of gas.
ASTRONOMY & ASTROPHYSICS
(2023)
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
S. E. van Terwisga, A. Hacar
Summary: External far-ultraviolet (FUV) irradiation has a significant impact on the evolution of protoplanetary disks. This study used a large sample from the SODA survey to investigate the effects of intermediate FUV radiation fields in L1641 and L1647. The results show that the median disk mass in the most irradiated disks decreases by a factor of 2, and the 95th percentile of disk masses decreases by a factor of 4 over a range of radiation fields from 1 to 100G(0). This effect is present in multiple populations of stars and localized within 2pc of ionizing stars. An empirical irradiation-disk mass relation is derived for the first time.
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
C. Gieser, H. Beuther, E. F. van Dishoeck, L. Francis, M. L. van Gelder, L. Tychoniec, P. J. Kavanagh, G. Perotti, A. Caratti o Garatti, T. P. Ray, P. Klaassen, K. Justtanont, H. Linnartz, W. R. M. Rocha, K. Slavicinska, L. Colina, M. Gudel, Th. Henning, P. -O. Lagage, G. Ostlin, B. Vandenbussche, C. Waelkens, G. Wright
Summary: The study focuses on the high-mass star-forming region IRAS 23385, investigating warm and cold gas components using high-angular-resolution mid-infrared and millimeter observations. The results show a strong connection between warm and cold gas, with outflows traced by mid-infrared H-2 lines having molecular counterparts in the millimeter regime. Despite multiple powerful outflows causing dense and hot shocks, a cold dense envelope allows star formation to proceed. Further research with JWST is needed to fully understand the spatially resolved mid-infrared properties of low- and high-mass protostars.
ASTRONOMY & ASTROPHYSICS
(2023)
Article
Astronomy & Astrophysics
Jeong-Eun Lee, Giseon Baek, Seokho Lee, Jae-Hong Jeong, Chul-Hwan Kim, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, John J. Tobin
Summary: We present the spectra of complex organic molecules (COMs) detected in HOPS 373SW using the ALMA. The observation reveals the extremely young chemical characteristics and strong deuteration of methanol in HOPS 373SW. Comparisons with other hot corinos suggest that HOPS 373SW is in a very early evolutionary stage. The detection of COMs in HOPS 373SW presents an important opportunity to study surface chemistry in the cold prestellar phase.
ASTROPHYSICAL JOURNAL
(2023)
Article
Astronomy & Astrophysics
Jinshi (Insa Choi) Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jorgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaria-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Summary: In this study, the Class 0/I protostellar system Ced110 IRS4 was observed using ALMA, revealing it as a binary system with a separation of 250 au. The continuum emission from the main source and its companion indicates disk-like structures, likely dust disks. The main source Ced110 IRS4A shows a disk-like structure with bumps along its major axis.
ASTROPHYSICAL JOURNAL
(2023)
Article
Astronomy & Astrophysics
Miyu Kido, Shigehisa Takakuwa, Kazuya Saigo, Nagayoshi Ohashi, John J. Tobin, Jes K. Jorgensen, Yuri Aikawa, Yusuke Aso, Frankie J. Encalada, Christian Flores, Sacha Gavino, Itziar de Gregorio-Monsalvo, Ilseung Han, Shingo Hirano, Patrick M. Koch, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Shoji Mori, Suchitra Narayanan, Adele L. Plunkett, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Alejandro Santamaria-Miranda, Rajeeb Sharma, Patrick D. Sheehan, Travis J. Thieme, Kengo Tomida, Merel L. R. van 't Hoff, Jonathan P. Williams, Yoshihide Yamato, Hsi-Wei Yen
Summary: We report observations of Class 0 protostar IRAS 16544-1604 in CB 68 using ALMA's Early Planet Formation in Embedded Disks (eDisk) program. The observations reveal a dusty protostellar disk with a radius of about 30 au, seen close to edge-on, and asymmetric structures along both major and minor axes. Gas in the disk follows a Keplerian rotation pattern, and there are streamer-like features connecting from different directions to the disk, as well as bending outflows. The detection of specific molecules at the tip of one streamer suggests the presence of accretion shocks.
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)
Proceedings Paper
Computer Science, Artificial Intelligence
Michele Delli Veneri, Lukasz Tychoniec, Fabrizia Guglielmetti, Eric Villard, Giuseppe Longo
Summary: We propose a Deep Learning pipeline for detecting astronomical sources in radiointerferometric simulated data cubes. The pipeline consists of two Deep Learning models: a Convolutional Autoencoder for spatial detection of sources, and a RNN for denoising and detecting emission peaks in the frequency domain. By combining spatial and frequency information, the pipeline achieves higher completeness and eliminates false positives. It performs better and has faster execution times compared to traditional methods, detecting 92% of sources up to 1.31 Jy/beam flux with no false positives, making it a reliable solution for future astronomical radio surveys.
MACHINE LEARNING AND PRINCIPLES AND PRACTICE OF KNOWLEDGE DISCOVERY IN DATABASES, ECML PKDD 2022, PT I
(2023)