Author:
Dominik C.,Dullemond C.P.
Abstract
A leading paradigm in planet formation is currently the streaming
instability and pebble accretion scenario. Notably, dust
must grow into sizes in a specific regime of Stokes numbers in
order to make the processes in the scenario viable and sufficiently
effective. The dust growth models currently in use do not
implement some of the growth barriers suggested to be relevant in
the literature. We investigate if the bouncing barrier, when effective, has
an impact on the timescales and efficiencies of processes such as the
streaming instability and pebble accretion as well as on the
observational appearance of planet-forming disks. We implemented a formalism for the bouncing barrier into the publicly
available dust growth model DustPy and ran a series of
models to understand the impact. We found that the bouncing barrier has a significant effect on the dust
evolution in planet-forming disks. In many cases, it reduces the
size of the typical or largest particles available in the disk; it
produces a very narrow, almost monodisperse, size distribution; and
it removes most grains in the process, with an impact on scattered light images. It modifies the settling and therefore the effectiveness of and timescales for the streaming instability and for pebble accretion. An active bouncing barrier may well
have observational consequences: It may reduce the strength of
the signatures of small particles (e.g., the 10 silicate
feature), and it may create additional shadowed regions visible
in scattered light images. Modeling of planet formation that leans heavily on the streaming
instability and on pebble accretion should take the bouncing
barrier into account. The complete removal of small grains in
our model is not consistent with observations. However, this
could be resolved by incomplete vertical mixing or some level of
erosion in collisions.
Funder
Deutsche Forschungsgemeinschaft
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
4 articles.
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