A5017314420- Astrophysics and Star Formation Studies
- Astro and Planetary Science
- Molecular Spectroscopy and Structure
- Stellar, planetary, and galactic studies
- Atmospheric Ozone and Climate
- Advanced Combustion Engine Technologies
- Phase Equilibria and Thermodynamics
- Fluid Dynamics and Turbulent Flows
- Solar and Space Plasma Dynamics
- Spacecraft Dynamics and Control
- Laser-induced spectroscopy and plasma
- Thermodynamic properties of mixtures
- Quantum chaos and dynamical systems
- Advanced Thermodynamic Systems and Engines
- Planetary Science and Exploration
- Astrophysical Phenomena and Observations
University of Copenhagen
2022-2024
Laboratoire d'Astrophysique de Bordeaux
2021
Université de Bordeaux
2021
Centre National de la Recherche Scientifique
2021
We present an overview of the Large Program, ``Early Planet Formation in Embedded Disks (eDisk)'', conducted with Atacama Millimeter/submillimeter Array (ALMA). The ubiquitous detections substructures, particularly rings and gaps, protoplanetary disks around T Tauri stars raise possibility that at least some planet formation may have already started during embedded stages star formation. In order to address exactly how when is initiated, program focuses on searching for substructures 12...
Abstract While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how settles the midplane unclear. As part of Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks, we analyze edge-on, embedded, I protostar IRAS 04302+2247, also nicknamed “Butterfly Star.” With a resolution 0.″05 (8 au), 1.3 mm continuum shows an asymmetry along minor axis that is evidence thick geometrically disk viewed nearly...
Abstract We present observations of the Class 0 protostar IRAS 16544–1604 in CB 68 from “Early Planet Formation Embedded Disks (eDisk)” ALMA Large program. The target continuum and lines at 1.3 mm with an angular resolution ∼5 au. image reveals a dusty protostellar disk radius ∼30 au seen close to edge-on asymmetric structures along both major minor axes. While asymmetry axis can be interpreted as effect dust flaring, comes real nonaxisymmetric structure. C 18 O cubes clearly show gas that...
Studying the physical and chemical conditions of young embedded disks is crucial to constrain initial for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations dust continuum at $\sim$0.06" (8 au) resolution molecular line emission $\sim$0.17" (24 toward Class 0 protostar L1527 IRS from Program eDisk (Early Planet Formation in Embedded Disks). The smooth without substructures, but asymmetric along both major minor axes disk as previously...
Abstract We performed radiative transfer calculations and observing simulations to reproduce the 1.3 mm dust-continuum C 18 O (2–1) images in Class I protostar R CrA IRS7B-a, observed with ALMA Large Program “Early Planet Formation Embedded Disks (eDisk).” found that a dust disk model passively heated by central cannot peak brightness temperature of continuum emission (∼195 K), regardless assumptions about opacity. Our calculation suggests viscous accretion heating is required high...
Aims. The ability of bulk ices (H 2 O, CO ) to trap volatiles has been well studied in any experimental sense, but largely ignored protoplanetary disk and planet formation models as the interpretation their observations. We demonstrate influence volatile trapping on C/O ratios planet-forming environments. Methods. created a simple model CO, , H O snowlines disks calculated ratio at different radii temperatures. included factor, which partially inhibits release (CO, snowline releases them...
Abstract We present high-resolution Karl G. Jansky Very Large Array (VLA) observations of the protostar L1527 IRS at 7 mm, 1.3 cm, and 2 cm wavelengths. detect edge-on dust disk all three wavelengths find that it is asymmetric, with southern side brighter than northern side. confirm this asymmetry through analytic modeling also flared mm. test data against models including gap features in intensity profile, though we cannot rule such out, they do not provide a statistically significant...
We present high-resolution, high-sensitivity observations of the Class 0 protostar RCrA IRS5N as part Atacama Large Milimeter/submilimeter Array (ALMA) large program Early Planet Formation in Embedded Disks (eDisk). The 1.3 mm continuum emission reveals a flattened structure around IRS5N, consistent with protostellar disk early phases evolution. appears smooth and shows no substructures. However, brightness asymmetry is observed along minor axis disk, suggesting optically geometrically...
Grain surface chemistry is key to the composition of protoplanetary disks around young stars. The temperature grains depends on their size. We evaluate impact this dependence disk chemistry. model a moderately massive with 16 different grain sizes. use POLARIS calculate dust temperatures and local UV flux. using 3-phase astrochemical code NAUTILUS. Photoprocesses are handled frequency-dependent cross-sections, new method account for self mutual shielding. multi-grain outputs compared those...
The ability of bulk ices (H$_{2}$O, CO$_{2}$) to trap volatiles has been well studied in any experimental sense, but largely ignored protoplanetary disk and planet formation models as the interpretation their observations. We demonstrate influence volatile trapping on C/O ratios planet-forming environments. created a simple model CO, CO$_{2}$, H$_{2}$O snowlines disks calculated ratio at different radii temperatures. included factor, which partially inhibits release (CO, snowline releases...
Icy dust particles emerge in star-forming clouds and are subsequently incorporated protoplanetary disks, where they coagulate into larger pebbles up to millimeter size. In the disk midplane, ices shielded from UV radiation, but moderate levels of turbulence can lift small surface, be altered, or destroyed. Nevertheless, studies comets meteorites generally find that at least partly retain their interstellar medium (ISM) composition before being accreted onto these minor bodies. We modeled...
Context. Characterizing the dust thermal structure in protoplanetary disks is a fundamental task because surface temperature can affect both planetary formation and chemical evolution. Because depends on many parameters, including grain size, it be challenging to properly model structure. Many chemistry disk models usually employ sophisticated single designed reproduce effect of realistic population presumably composed large diversity sizes. This generally represents good approximation most...
Recent observational missions have uncovered a significant number of compact multi-exoplanet systems. The tight orbital spacing these systems has led to much effort being applied the understanding their stability; however, key limitation majority studies is termination simulations as soon orbits two planets cross. In this work we explore stability compact, three-planet and continue our all way first collision yield better lifetime We perform over $25,000$ integrations Sun-like star orbited...
We performed radiative transfer calculations and observing simulations to reproduce the 1.3-mm dust-continuum C$^{18}$O (2-1) images in Class I protostar R CrA IRS7B-a, observed with ALMA Large Program ``Early Planet Formation Embedded Disks (eDisk)". found that dust disk model passively heated by central cannot peak brightness temperature of continuum emission ($\sim$195 K), regardless assumptions about opacity. Our calculation suggests viscous accretion heating is required high...
Abstract We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the binary Class 0 protostellar system BHR 71 IRS1 and IRS2 as part Early Planet Formation in Embedded Disks (eDisk) ALMA Program. describe 12 CO ( J = 2–1), 13 C 18 O H 2 3 2,1 –2 2,0 ), SiO 5–4) molecular lines along with 1.3 mm continuum at high spatial resolution (∼0.″08 or ∼5 au). Dust emission is detected toward IRS2, a central compact component extended emission. The components are smooth show no...
Icy dust particles emerge in star-forming clouds and are subsequently incorporated protoplanetary disks, where they coagulate into larger pebbles up to mm size. In the disk midplane, ices shielded from UV radiation, but moderate levels of turbulence can lift small surface, be altered, or destroyed. Nevertheless, studies comets meteorites generally find that at least partly retained their interstellar medium (ISM) composition before being accreted onto these minor bodies. Here we model this...
Studying the physical and chemical conditions of young embedded disks is crucial to constrain initial for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations dust continuum at $\sim$0.06" (8 au) resolution molecular line emission $\sim$0.17" (24 toward Class 0 protostar L1527 IRS from Program eDisk (Early Planet Formation in Embedded Disks). The smooth without substructures, but asymmetric along both major minor axes disk as previously...
We present an overview of the Large Program, ``Early Planet Formation in Embedded Disks (eDisk)'', conducted with Atacama Millimeter/submillimeter Array (ALMA). The ubiquitous detections substructures, particularly rings and gaps, protoplanetary disks around T Tauri stars raise possibility that at least some planet formation may have already started during embedded stages star formation. In order to address exactly how when is initiated, program focuses on searching for substructures 12...
While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how settles the midplane unclear. As part of Atacama Large Millimeter/submillimeter Array (ALMA) large program, Early Planet Formation in Embedded Disks, we analyze edge-on, embedded, I protostar IRAS 04302+2247, also nicknamed ``Butterfly Star." With a resolution 0.05" (8~au), 1.3 mm continuum shows an asymmetry along minor axis which is evidence thick geometrically disk viewed nearly...
We present observations of the Class 0 protostar IRAS 16544-1604 in CB 68 from ''Early Planet Formation Embedded Disks (eDisk)'' ALMA Large program. The target continuum and lines at 1.3-mm with an angular resolution $\sim$5 au. image reveals a dusty protostellar disk radius $\sim$30 au seen close to edge-on, asymmetric structures both along major minor axes. While asymmetry axis can be interpreted as effect dust flaring, comes real non-axisymmetric structure. C$^{18}$O cubes clearly show...
Characterizing the dust thermal structure in protoplanetary disks is a fundamental task as surface temperature can affect both planetary formation and chemical evolution. Since dependent on many parameters, including grain size, properly modeling be challenging. Many chemistry disk models usually employ sophisticated single designed to reproduce effect of realistic population presumably composed large diversity sizes. This generally represents good approximation most cases. Nonetheless, this...