On the Dust Signatures Induced by Eccentric Super-Earths in Protoplanetary Disks. (arXiv:1910.03130v1 [astro-ph.EP])

On the Dust Signatures Induced by Eccentric Super-Earths in Protoplanetary Disks. (arXiv:1910.03130v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Ya-Ping Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hui Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_S/0/1/0/all/0/1">Shengtai Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_D/0/1/0/all/0/1">Douglas N. C. Lin</a> (2) ((1) LANL, (2) UCSC)

We investigate the impact of a highly eccentric 10 $M_{rm oplus}$ (where
$M_{rm oplus}$ is the Earth mass) planet embedded in a dusty protoplanetary
disk on the dust dynamics and its observational implications. By carrying out
high-resolution 2D gas and dust two-fluid hydrodynamical simulations, we find
that the planet’s orbit can be circularized at large radii. After the planet’s
orbit is circularized, partial gap opening and dust ring formation happen close
to the planet’s circularization radius, which can explain the observed
gaps/rings at the outer region of disks. When the disk mass and viscosity
become low, we find that an eccentric planet can even open gaps and produce
dust rings close to the pericenter and apocenter radii before its
circularization. This offers alternative scenarios for explaining the observed
dust rings and gaps in protoplanetary disks. A lower disk viscosity is favored
to produce brighter rings in observations. An eccentric planet can also
potentially slow down the dust radial drift in the outer region of the disk
when the disk viscosity is low ($alpha lesssim2times10^{-4}$) and the
circularization is faster than the dust radial drift.

We investigate the impact of a highly eccentric 10 $M_{rm oplus}$ (where
$M_{rm oplus}$ is the Earth mass) planet embedded in a dusty protoplanetary
disk on the dust dynamics and its observational implications. By carrying out
high-resolution 2D gas and dust two-fluid hydrodynamical simulations, we find
that the planet’s orbit can be circularized at large radii. After the planet’s
orbit is circularized, partial gap opening and dust ring formation happen close
to the planet’s circularization radius, which can explain the observed
gaps/rings at the outer region of disks. When the disk mass and viscosity
become low, we find that an eccentric planet can even open gaps and produce
dust rings close to the pericenter and apocenter radii before its
circularization. This offers alternative scenarios for explaining the observed
dust rings and gaps in protoplanetary disks. A lower disk viscosity is favored
to produce brighter rings in observations. An eccentric planet can also
potentially slow down the dust radial drift in the outer region of the disk
when the disk viscosity is low ($alpha lesssim2times10^{-4}$) and the
circularization is faster than the dust radial drift.

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