Circumstellar dust distribution in systems with two planets in resonance. (arXiv:1812.07698v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Marzari_F/0/1/0/all/0/1">Francesco Marzari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAngelo_G/0/1/0/all/0/1">Gennaro D'Angelo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Picogna_G/0/1/0/all/0/1">Giovanni Picogna</a>
We investigate via numerical modeling the effects of two planets locked in
resonance, and migrating outward, on the dust distribution of the natal
circumstellar disk. We aim to test whether the dust distribution exhibits
peculiar features arising from the interplay among the gravitational
perturbations of the planets in resonance, the evolution of the gas, and its
influence on the dust grains’ dynamics. We focus on the 3:2 and 2:1 resonance,
where the trapping may be caused by the convergent migration of a Jupiter- and
Saturn-mass planet, preceding the common gap formation and ensuing outward (or
inward) migration. Models show that a common gap also forms in the dust
component — similarly to what a single, more massive planet would generate —
and that outward migration leads to a progressive widening of the dust gap and
to a decoupling from the gas gap. As the system evolves, a significantly wider
gap is observed in the dust distribution, which ceases to overlap with the gas
gap in the inner disk regions. At the outer edge of the gas gap, outward
migration of the planets produces an over-density of dust particles, which
evolve differently in the 3:2 and 2:1 resonances. For the 3:2, the dust trap at
the gap’s outer edge is partly efficient and a significant fraction of the
grains filters through the gap. For the 2:1 resonance, the trap is more
efficient and very few grains cross the gap, while the vast majority accumulate
at the outer edge of the gap.
We investigate via numerical modeling the effects of two planets locked in
resonance, and migrating outward, on the dust distribution of the natal
circumstellar disk. We aim to test whether the dust distribution exhibits
peculiar features arising from the interplay among the gravitational
perturbations of the planets in resonance, the evolution of the gas, and its
influence on the dust grains’ dynamics. We focus on the 3:2 and 2:1 resonance,
where the trapping may be caused by the convergent migration of a Jupiter- and
Saturn-mass planet, preceding the common gap formation and ensuing outward (or
inward) migration. Models show that a common gap also forms in the dust
component — similarly to what a single, more massive planet would generate —
and that outward migration leads to a progressive widening of the dust gap and
to a decoupling from the gas gap. As the system evolves, a significantly wider
gap is observed in the dust distribution, which ceases to overlap with the gas
gap in the inner disk regions. At the outer edge of the gas gap, outward
migration of the planets produces an over-density of dust particles, which
evolve differently in the 3:2 and 2:1 resonances. For the 3:2, the dust trap at
the gap’s outer edge is partly efficient and a significant fraction of the
grains filters through the gap. For the 2:1 resonance, the trap is more
efficient and very few grains cross the gap, while the vast majority accumulate
at the outer edge of the gap.
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