Nearly Polar orbit of the sub-Neptune HD3167 c: Constraints on a multi-planet system dynamical history. (arXiv:1906.11013v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dalal_S/0/1/0/all/0/1">Shweta Dalal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hebrard_G/0/1/0/all/0/1">Guillaume Hébrard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Etangs_A/0/1/0/all/0/1">Alain Lecavelier des Étangs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petit_A/0/1/0/all/0/1">Antoine C. Petit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourrier_V/0/1/0/all/0/1">Vincent Bourrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laskar_J/0/1/0/all/0/1">Jacques Laskar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Konig_P/0/1/0/all/0/1">Pierre-Cécil König</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Correia_A/0/1/0/all/0/1">Alexandre C. M. Correia</a>
We present the obliquity measurement i.e. the angle between the normal of the
planet orbital plane and stellar spin axis of the sub-Neptune planet HD3167 c
that transits a bright, nearby K0 star. New observations obtained with HARPS-N
at Telescopio Nazionale Galileo (TNG) are employed for our analysis. We study
the orbital architecture of this multi-planet system to understand its
dynamical history. We also put constraints on the obliquity of planet d from
the geometry of the planetary system and the dynamical study of the system. The
sky-projected obliquity is measured using three different methods, i.e
Rossiter-McLaughlin anomaly, Doppler tomography and Reloaded
Rossiter-McLaughlin techniques. We perform the stability analysis of the system
and investigate the dynamical interactions between the planets and star. HD3167
c is found to be nearly polar with sky-projected obliquity, $lambda$ =
-98$^{circ} pm$23$^{circ}$. This misalignment of the orbit of planet c with
the spin axis of the host star is detected with 97% confidence. The analysis of
the dynamics of this system yields coplanar orbits of planets c and d. It also
shows that it is unlikely that the currently observed system can, by itself,
generate such a large obliquity for planets c and d. However, the polar orbits
of planets c and d could be explained by the presence of an outer companion in
the system. Follow-up observations of the system are required to confirm such a
long period companion.
We present the obliquity measurement i.e. the angle between the normal of the
planet orbital plane and stellar spin axis of the sub-Neptune planet HD3167 c
that transits a bright, nearby K0 star. New observations obtained with HARPS-N
at Telescopio Nazionale Galileo (TNG) are employed for our analysis. We study
the orbital architecture of this multi-planet system to understand its
dynamical history. We also put constraints on the obliquity of planet d from
the geometry of the planetary system and the dynamical study of the system. The
sky-projected obliquity is measured using three different methods, i.e
Rossiter-McLaughlin anomaly, Doppler tomography and Reloaded
Rossiter-McLaughlin techniques. We perform the stability analysis of the system
and investigate the dynamical interactions between the planets and star. HD3167
c is found to be nearly polar with sky-projected obliquity, $lambda$ =
-98$^{circ} pm$23$^{circ}$. This misalignment of the orbit of planet c with
the spin axis of the host star is detected with 97% confidence. The analysis of
the dynamics of this system yields coplanar orbits of planets c and d. It also
shows that it is unlikely that the currently observed system can, by itself,
generate such a large obliquity for planets c and d. However, the polar orbits
of planets c and d could be explained by the presence of an outer companion in
the system. Follow-up observations of the system are required to confirm such a
long period companion.
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