Solid accretion onto planetary cores in radiative disks. (arXiv:2004.01745v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zormpas_A/0/1/0/all/0/1">Apostolos Zormpas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Picogna_G/0/1/0/all/0/1">Giovanni Picogna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ercolano_B/0/1/0/all/0/1">Barbara Ercolano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kley_W/0/1/0/all/0/1">Wilhelm Kley</a>
The solid accretion rate, necessary to grow gas giant planetary cores within
the disk lifetime, has been a major constraint for theories of planet
formation. We tested the solid accretion rate efficiency on planetary cores of
different masses embedded in their birth disk, by means of 3D
radiation-hydrodynamics, where we followed the evolution of a swarm of embedded
solids of different sizes. We found that using a realistic equation of state
and radiative cooling, the disk at 5 au is able to cool efficiently and reduce
its aspect ratio. As a result, the pebble isolation mass is reached before the
core grows to 10 Earth masses, stopping efficiently the pebble flux and
creating a transition disk. Moreover, the reduced isolation mass halts the
solid accretion before the core reaches the critical mass, leading to a barrier
to giant planet formation, and it explains the large abundance of super-Earth
planets in the observed population.
The solid accretion rate, necessary to grow gas giant planetary cores within
the disk lifetime, has been a major constraint for theories of planet
formation. We tested the solid accretion rate efficiency on planetary cores of
different masses embedded in their birth disk, by means of 3D
radiation-hydrodynamics, where we followed the evolution of a swarm of embedded
solids of different sizes. We found that using a realistic equation of state
and radiative cooling, the disk at 5 au is able to cool efficiently and reduce
its aspect ratio. As a result, the pebble isolation mass is reached before the
core grows to 10 Earth masses, stopping efficiently the pebble flux and
creating a transition disk. Moreover, the reduced isolation mass halts the
solid accretion before the core reaches the critical mass, leading to a barrier
to giant planet formation, and it explains the large abundance of super-Earth
planets in the observed population.
http://arxiv.org/icons/sfx.gif
