155 research outputs found
Science with an ngVLA: Resolved Substructures in Protoplanetary Disks
Terrestrial planets and the cores of giant planets are thought to be built by
the collisional agglomeration of solids spanning over 20 orders of magnitude in
size within a few million years. However, there is tension between this basic
picture of planet formation and standard theoretical assumptions associated
with the migration of "pebbles" (mm/cm-sized particles) in gas-rich disks
and the presumably much longer timescales necessary to assemble
(km-scale) "planetesimals". To confront these potential theoretical
discrepancies with observational constraints, the ideal tracer of the solids
concentrated in protoplanetary disk substructures is the 30-100 GHz continuum,
which strikes the best balance in sensitivity (emission still bright), optical
depth (low enough to reliably estimate densities), and angular resolution (high
enough to resolve fine-scale features at disk radii as small as 1 au). With its
combination of sensitivity, frequency coverage, and angular resolution, the
next-generation VLA will be the only facility that has the capabilities to open
up this new window into the physics of planetesimal formation.Comment: To be published in the ASP Monograph Series, Science with a
Next-Generation VLA, ed. E. J. Murphy (ASP, San Francisco, CA
The properties of the inner disk around HL Tau: Multi-wavelength modeling of the dust emission
We conducted a detailed radiative transfer modeling of the dust emission from
the circumstellar disk around HL Tau. The goal of our study is to derive the
surface density profile of the inner disk and its structure. In addition to the
Atacama Large Millimeter/submillimeter Array images at Band 3 (2.9mm), Band 6
(1.3mm), and Band 7 (0.87mm), the most recent Karl G. Jansky Very Large Array
(VLA) observations at 7mm were included in the analysis. A simulated annealing
algorithm was invoked to search for the optimum model. The radiative transfer
analysis demonstrates that most radial components (i.e., >6AU) of the disk
become optically thin at a wavelength of 7mm, which allows us to constrain, for
the first time, the dust density distribution in the inner region of the disk.
We found that a homogeneous grain size distribution is not sufficient to
explain the observed images at different wavelengths simultaneously, while
models with a shallower grain size distribution in the inner disk work well. We
found clear evidence that larger grains are trapped in the first bright ring.
Our results imply that dust evolution has already taken place in the disk at a
relatively young (i.e., ~1Myr) age. We compared the midplane temperature
distribution, optical depth, and properties of various dust rings with those
reported previously. Using the Toomre parameter, we briefly discussed the
gravitational instability as a potential mechanism for the origin of the dust
clump detected in the first bright ring via the VLA observations.Comment: Accepted for publication in A&A (10 pages
Characterizing the dust content of disk substructures in TW Hya
We present Atacama Large Millimeter Array (ALMA) observations of TW Hya at
3.1 mm with milliarcsecond resolution. These new data were combined
with archival high angular resolution ALMA observations at 0.87 mm, 1.3 mm, and
2.1 mm. We analyze these multi-wavelength data to infer a disk radial profile
of the dust surface density, maximum particle size, and slope of the particle
size distribution. Most previously known annular substructures in the disk of
TW Hya are resolved at the four wavelengths. Inside the inner 3 au cavity, the
2.1 mm and 3.1 mm images show a compact source of free-free emission, likely
associated with an ionized jet. Our multi-wavelength analysis of the dust
emission shows that the maximum particle size in the disk of TW Hya is mm.
The inner 20 au are completely optically thick at all four bands, which results
in the data tracing different disk heights at different wavelengths. Coupled
with the effects of dust settling, this prevents the derivation of accurate
density and grain size estimates in these regions. At au, we find
evidence of the accumulation of large dust particle at the position of the
bright rings, indicating that these are working as dust traps. The total dust
mass in the disk is between 250 and 330 , which represents a
gas-to-dust mass ratio between 50 and 70. Our mass measurement is a factor of
4.5-5.9 higher than the mass that one would estimate using the typical
assumptions of large demographic surveys. Our results indicate that the ring
substructures in TW Hya are ideal locations to trigger the streaming
instability and form new generations of planetesimals.Comment: 22 pages, 17 figures, accepted for publication in A&A. Language
edited versio
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