The Origin of Kepler-419b: A Path to Tidal Migration Via Four-body Secular Interactions. (arXiv:1902.05144v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Jackson_J/0/1/0/all/0/1">Jonathan M. Jackson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_R/0/1/0/all/0/1">Rebekah I. Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zalesky_J/0/1/0/all/0/1">Joseph Zalesky</a>
We test the high-eccentricity tidal migration scenario for Kepler-419b, a
member of the eccentric warm Jupiter class of planets whose origin is debated.
Kepler-419 hosts two known planets (b,c). However, in its current
configuration, planet c cannot excite the eccentricity of planet b enough to
undergo high-eccentricity tidal migration. We investigate whether the presence
of an undiscovered fourth body could explain the orbit of Kepler-419b. We
explore the parameter space of this potential third giant planet using a suite
of N-body simulations with a range of initial conditions. From the results of
these simulations, coupled with observational constraints, we can rule out this
mechanism for much of the parameter space of initial object d conditions.
However, for a small range of parameters (masses between 0.5 and 7
$m_{rm{Jup}}$, semi-major axes between 4 and 7.5 AU, eccentricities between
0.18 and 0.35, and mutual inclinations near 0$^{circ}$) an undiscovered object
d could periodically excite the eccentricity of Kepler-419b without
destabilizing the system over 1 Gyr while producing currently undetectable
radial velocity and transit timing variation signals.
We test the high-eccentricity tidal migration scenario for Kepler-419b, a
member of the eccentric warm Jupiter class of planets whose origin is debated.
Kepler-419 hosts two known planets (b,c). However, in its current
configuration, planet c cannot excite the eccentricity of planet b enough to
undergo high-eccentricity tidal migration. We investigate whether the presence
of an undiscovered fourth body could explain the orbit of Kepler-419b. We
explore the parameter space of this potential third giant planet using a suite
of N-body simulations with a range of initial conditions. From the results of
these simulations, coupled with observational constraints, we can rule out this
mechanism for much of the parameter space of initial object d conditions.
However, for a small range of parameters (masses between 0.5 and 7
$m_{rm{Jup}}$, semi-major axes between 4 and 7.5 AU, eccentricities between
0.18 and 0.35, and mutual inclinations near 0$^{circ}$) an undiscovered object
d could periodically excite the eccentricity of Kepler-419b without
destabilizing the system over 1 Gyr while producing currently undetectable
radial velocity and transit timing variation signals.
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