Kavli Affiliate: Ruobing Dong
| First 5 Authors: Jun Hashimoto, Jun Hashimoto, , ,
| Summary:
The maximum grain size in protoplanetary disks is a critical parameter for
planet formation, as the efficiency of mechanisms like streaming instability
and pebble accretion depend on grain size. Even young class 0/I objects, such
as HL Tau, show substructures in their disks, indicating the potential for
early planet formation. In this study, we investigated the grain size in the
dust surrounding the class I object WL 17 using the Karl G. Jansky Very Large
Array. Observations were conducted across seven frequency bands (Q, Ka, K, Ku,
X, C, and S bands) ranging from 2 to 48 GHz, corresponding to wavelengths of 15
cm to 6.3 mm, with a spatial resolution exceeding 0farcs5. While the ring
structure at 0farcs1 of WL 17 remains unresolved in our data, its emission is
clearly detected at all observed frequencies, except at 2 GHz. To estimate the
maximum grain size ($a_rm max$) within the ring, we compared the observed
spectral energy distribution (SED) with theoretical SEDs calculated for various
$a_rm max$ values using radiative transfer models. Assuming the dust opacity
follows the DSHARP model, our analysis suggests that certain structures
internal to the ring achieved a maximum grain size of approximately 4.2 mm.
Additionally, we discuss the gravitational stability of the ring and the
potential planetary core mass that could form through pebble accretion within
the structure.
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