HD 110067 C Has an Aligned Orbit

J. Zak,H. M. J. Boffin,E. Sedaghati, A. Bocchieri,Q. Changeat,A. Fukui,A. Hatzes,T. Hillwig,K. Hornoch,D. Itrich,V. D. Ivanov,D. Jones,P. Kabath,Y. Kawai,L. V. Mugnai,F. Murgas,N. Narita,E. Palle,E. Pascale,P. Pravec,S. Redfield, G. Roccetti, M. Roth, J. Srba, Q. Tian,A. Tsiaras,D. Turrini,J. P. Vignes

ASTRONOMY & ASTROPHYSICS（2024）

Cited 0|Views22

Abstract

Planetary systems in mean motion resonances hold a special place among the planetary population. They allow us to study planet formation in great detail as dissipative processes are thought to have played an important role in their existence. Additionally, planetary masses in bright resonant systems can be independently measured via both radial velocities and transit timing variations. In principle, they also allow us to quickly determine the inclination of all planets in the system since, for the system to be stable, they are likely all in coplanar orbits. To describe the full dynamical state of the system, we also need the stellar obliquity, which provides the orbital alignment of a planet with respect to the spin of its host star and can be measured thanks to the Rossiter-McLaughlin effect. It was recently discovered that HD 110067 harbors a system of six sub-Neptunes in resonant chain orbits. We here analyze an ESPRESSO high-resolution spectroscopic time series of HD 110067 during the transit of planet c. We find the orbit of HD 110067 c to be well aligned, with a sky-projected obliquity of lambda =6(-26)(+24) deg. This result indicates that the current architecture of the system was reached through convergent migration without any major disruptive events. Finally, we report transit-timing variation in this system as we find a significant offset of 19 +/- 4 min in the center of the transit compared to the published ephemeris.

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Key words

techniques: radial velocities,planets and satellites: gaseous planets,planet-star interactions,planets and satellites: individual: HD 110067

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