The HD 181433 Planetary System: Dynamics and a New Orbital Solution. (arXiv:1906.05525v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Horner_J/0/1/0/all/0/1">Jonathan Horner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wittenmyer_R/0/1/0/all/0/1">Robert A Wittenmyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_D/0/1/0/all/0/1">Duncan J Wright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hinse_T/0/1/0/all/0/1">Tobias C Hinse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_J/0/1/0/all/0/1">Jonathan P Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kane_S/0/1/0/all/0/1">Stephen R Kane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clark_J/0/1/0/all/0/1">Jake T Clark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mengel_M/0/1/0/all/0/1">Matthew Mengel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agnew_M/0/1/0/all/0/1">Matthew T Agnew</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johns_D/0/1/0/all/0/1">Daniel Johns</a>
We present a detailed analysis of the orbital stability of the HD 181433
planetary system, finding it to exhibit strong dynamical instability across a
wide range of orbital eccentricities, semi-major axes, and mutual inclinations.
We also analyse the behaviour of an alternative system architecture, proposed
by Campanella (2011), and find that it offers greater stability than the
original solution, as a result of the planets being trapped in strong mutual
resonance.
We take advantage of more recent observations to perform a full refit of the
system, producing a new planetary solution. The best-fit orbit for HD 181433 d
now places the planet at a semi-major axis of 6.60$pm$0.22 au, with an
eccentricity of 0.469$pm$0.013. Extensive simulations of this new system
architecture reveal it to be dynamically stable across a broad range of
potential orbital parameter space, increasing our confidence that the new
solution represents the ground truth of the system.
Our work highlights the advantage of performing dynamical simulations of
candidate planetary systems in concert with the orbital fitting process, as
well as supporting the continuing monitoring of radial velocity planet search
targets.
We present a detailed analysis of the orbital stability of the HD 181433
planetary system, finding it to exhibit strong dynamical instability across a
wide range of orbital eccentricities, semi-major axes, and mutual inclinations.
We also analyse the behaviour of an alternative system architecture, proposed
by Campanella (2011), and find that it offers greater stability than the
original solution, as a result of the planets being trapped in strong mutual
resonance.
We take advantage of more recent observations to perform a full refit of the
system, producing a new planetary solution. The best-fit orbit for HD 181433 d
now places the planet at a semi-major axis of 6.60$pm$0.22 au, with an
eccentricity of 0.469$pm$0.013. Extensive simulations of this new system
architecture reveal it to be dynamically stable across a broad range of
potential orbital parameter space, increasing our confidence that the new
solution represents the ground truth of the system.
Our work highlights the advantage of performing dynamical simulations of
candidate planetary systems in concert with the orbital fitting process, as
well as supporting the continuing monitoring of radial velocity planet search
targets.
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