Dust growth and evolution in protoplanetary disks
Annual Review of Astronomy and Astrophysics(2023)
摘要
Over the past decade, advancement of observational capabilities, specifically
the Atacama Large Millimeter/submillimeter Array (ALMA) and SPHERE instrument,
alongside theoretical innovations like pebble accretion, have reshaped our
understanding of planet formation and the physics of protoplanetary disks.
Despite this progress, mysteries persist along the winded path of
micrometer-sized dust, from the interstellar medium, through transport and
growth in the protoplanetary disk, to becoming gravitationally bound bodies.
This review outlines our current knowledge of dust evolution in circumstellar
disks, yielding the following insights:
$\bullet$ Theoretical and laboratory studies have accurately predicted the
growth of dust particles to sizes that are susceptible to accumulation through
transport processes like radial drift and settling.
$\bullet$ Critical uncertainties in that process remain the level of
turbulence, the threshold collision velocities at which dust growth stalls, and
the evolution of dust porosity.
$\bullet$ Symmetric and asymmetric substructure are widespread. Dust traps
appear to be solving several long-standing issues in planet formation models,
and they are observationally consistent with being sites of active planetesimal
formation.
$\bullet$ In some instances, planets have been identified as the causes
behind substructures. This underlines the need to study earlier stages of disks
to understand how planets can form so rapidly.
In the future, better probes of the physical conditions in optically thick
regions, including densities, turbulence strength, kinematics, and particle
properties will be essential for unraveling the physical processes at play.
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