Planetary Embryo Collisions and the Wiggly Nature of Extreme Debris Disks. (arXiv:2101.05106v2 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Watt_L/0/1/0/all/0/1">Lewis Watt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leinhardt_Z/0/1/0/all/0/1">Zoë Leinhardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Su_K/0/1/0/all/0/1">Kate Su</a>
In this paper, we present results from a multi-stage numerical campaign to
begin to explain and determine why extreme debris disk detections are rare,
what types of impacts will result in extreme debris disks and what we can learn
about the parameters of the collision from the extreme debris disks. We begin
by simulating many giant impacts using a smoothed particle hydrodynamical code
with tabulated equations of state and track the escaping vapour from the
collision. Using an $N$-body code, we simulate the spatial evolution of the
vapour generated dust post-impact.
We show that impacts release vapour anisotropically not isotropically as has
been assumed previously and that the distribution of the resulting generated
dust is dependent on the mass ratio and impact angle of the collision. In
addition, we show that the anisotropic distribution of post-collision dust can
cause the formation or lack of formation of the short-term variation in flux
depending on the orientation of the collision with respect to the orbit around
the central star. Finally, our results suggest that there is a narrow region of
semi-major axis where a vapour generated disk would be observable for any
significant amount of time implying that giant impacts where most of the
escaping mass is in vapour would not be observed often but this does not mean
that the collisions are not occurring.
In this paper, we present results from a multi-stage numerical campaign to
begin to explain and determine why extreme debris disk detections are rare,
what types of impacts will result in extreme debris disks and what we can learn
about the parameters of the collision from the extreme debris disks. We begin
by simulating many giant impacts using a smoothed particle hydrodynamical code
with tabulated equations of state and track the escaping vapour from the
collision. Using an $N$-body code, we simulate the spatial evolution of the
vapour generated dust post-impact.
We show that impacts release vapour anisotropically not isotropically as has
been assumed previously and that the distribution of the resulting generated
dust is dependent on the mass ratio and impact angle of the collision. In
addition, we show that the anisotropic distribution of post-collision dust can
cause the formation or lack of formation of the short-term variation in flux
depending on the orientation of the collision with respect to the orbit around
the central star. Finally, our results suggest that there is a narrow region of
semi-major axis where a vapour generated disk would be observable for any
significant amount of time implying that giant impacts where most of the
escaping mass is in vapour would not be observed often but this does not mean
that the collisions are not occurring.
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