History of the solar nebula from meteorite paleomagnetism
We review recent advances in our understanding of magnetism in the solar nebula and
protoplanetary disks (PPDs). We discuss the implications of theory, meteorite …
protoplanetary disks (PPDs). We discuss the implications of theory, meteorite …
Interferometric observations of magnetic fields in forming stars
CLH Hull, Q Zhang - Frontiers in Astronomy and Space Sciences, 2019 - frontiersin.org
The magnetic field is a key ingredient in the recipe of star formation. However, the
importance of the magnetic field in the early stages of the formation of low-and high-mass …
importance of the magnetic field in the early stages of the formation of low-and high-mass …
The disk substructures at high angular resolution project (DSHARP). VII. The planet–disk interactions interpretation
Abstract The Disk Substructures at High Angular Resolution Project (DSHARP) provides a
large sample of protoplanetary disks with substructures that could be induced by young …
large sample of protoplanetary disks with substructures that could be induced by young …
The radial distribution of dust particles in the HL Tau disk from ALMA and VLA observations
C Carrasco-González, A Sierra, M Flock… - The Astrophysical …, 2019 - iopscience.iop.org
Understanding planet formation requires one to discern how dust grows in protoplanetary
disks. An important parameter to measure in disks is the maximum dust grain size present …
disks. An important parameter to measure in disks is the maximum dust grain size present …
Characterizing the dust content of disk substructures in TW Hydrae
E Macías, O Guerra-Alvarado… - Astronomy & …, 2021 - aanda.org
Context. A key piece of information to understand the origin and role of protoplanetary disk
substructures is their dust content. In particular, disk substructures associated with gas …
substructures is their dust content. In particular, disk substructures associated with gas …
Radiation hydrodynamical turbulence in protoplanetary disks: Numerical models and observational constraints
M Flock, RP Nelson, NJ Turner… - The Astrophysical …, 2017 - iopscience.iop.org
Planets are born in protostellar disks, which are now observed with enough resolution to
address questions about internal gas flows. Magnetic forces are possibly drivers of the flows …
address questions about internal gas flows. Magnetic forces are possibly drivers of the flows …
One solution to the mass budget problem for planet formation: optically thick disks with dust scattering
Abstract Atacama Large Millimeter Array (ALMA) surveys have suggested that the dust in
Class II disks may not be enough to explain the averaged solid mass in exoplanets, under …
Class II disks may not be enough to explain the averaged solid mass in exoplanets, under …
Multiple disk gaps and rings generated by a single super-Earth. II. Spacings, depths, and number of gaps, with application to real systems
Abstract The Atacama Large Millimeter/submillimeter Array (ALMA) has found multiple dust
gaps and rings in a number of protoplanetary disks in continuum emission at millimeter …
gaps and rings in a number of protoplanetary disks in continuum emission at millimeter …
Dust enrichment and grain growth in a smooth disk around the DG Tau protostar revealed by ALMA triple bands frequency observations
Characterizing the physical properties of dust grains in a protoplanetary disk is critical to
comprehending the planet formation process. Our study presents Atacama Large Millimeter …
comprehending the planet formation process. Our study presents Atacama Large Millimeter …
ALMA observations of polarized emission toward the CW Tau and DG Tau protoplanetary disks: constraints on dust grain growth and settling
F Bacciotti, JM Girart, M Padovani… - The Astrophysical …, 2018 - iopscience.iop.org
We present polarimetric data of CW Tau and DG Tau, two well-known Class II disk/jet
systems, obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at 870 μm …
systems, obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at 870 μm …