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The hot Neptune WASP-166 b with ESPRESSO – I. Refining the planetary architecture and stellar variability
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(2022) The hot Neptune WASP-166 b with ESPRESSO – I. Refining the planetary architecture and stellar variability. Monthly Notices of the Royal Astronomical Society, 516 (1). pp. 298-315. doi:10.1093/mnras/stac2178 ISSN 1745-3933.
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WRAP-The-hot-Neptune-WASP-166-b-with-ESPRESSO-I-Refining-the-planetary-architecture-and-stellar-variability-Doyle-2022.pdf - Published Version - Requires a PDF viewer. Available under License Creative Commons Attribution 4.0. Download (2789Kb) | Preview |
Official URL: http://dx.doi.org/10.1093/mnras/stac2178
Abstract
In this paper, we present high-resolution spectroscopic transit observations from ESPRESSO of the super-Neptune WASP-166 b. In addition to spectroscopic ESPRESSO data, we analyse photometric data from TESS of six WASP-166 b transits along with simultaneous NGTS observations of the ESPRESSO runs. These observations were used to fit for the planetary parameters as well as assessing the level of stellar activity (e.g. spot crossings, flares) present during the ESPRESSO observations. We utilize the reloaded Rossiter McLaughlin (RRM) technique to spatially resolve the stellar surface, characterizing the centre-to-limb convection-induced variations, and to refine the star–planet obliquity. We find WASP-166 b has a projected obliquity of λ=−15.52+2.85−2.76∘ and vsin (i) = 4.97 ± 0.09 km s−1 which is consistent with the literature. We were able to characterize centre-to-limb convective variations as a result of granulation on the surface of the star on the order of a few km s−1 for the first time. We modelled the centre-to-limb convective variations using a linear, quadratic, and cubic model with the cubic being preferred. In addition, by modelling the differential rotation and centre-to-limb convective variations simultaneously, we were able to retrieve a potential antisolar differential rotational shear (α ∼ −0.5) and stellar inclination (i* either 42.03+9.13−9.60∘ or 133.64+8.42−7.98∘ if the star is pointing towards or away from us). Finally, we investigate how the shape of the cross-correlation functions change as a function of limb angle and compare our results to magnetohydrodynamic simulations.
| Item Type: | Journal Article | |||||||||||||||||||||||||||
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| Subjects: | Q Science > QB Astronomy | |||||||||||||||||||||||||||
| Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | |||||||||||||||||||||||||||
| Library of Congress Subject Headings (LCSH): | Astronomical photometry, Stellar activity , Magnetohydrodynamics , Stars -- Magnetic fields | |||||||||||||||||||||||||||
| Journal or Publication Title: | Monthly Notices of the Royal Astronomical Society | |||||||||||||||||||||||||||
| Publisher: | Oxford University Press | |||||||||||||||||||||||||||
| ISSN: | 1745-3933 | |||||||||||||||||||||||||||
| Official Date: | October 2022 | |||||||||||||||||||||||||||
| Dates: |
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| Volume: | 516 | |||||||||||||||||||||||||||
| Number: | 1 | |||||||||||||||||||||||||||
| Page Range: | pp. 298-315 | |||||||||||||||||||||||||||
| DOI: | 10.1093/mnras/stac2178 | |||||||||||||||||||||||||||
| Status: | Peer Reviewed | |||||||||||||||||||||||||||
| Publication Status: | Published | |||||||||||||||||||||||||||
| Access rights to Published version: | Open Access (Creative Commons) | |||||||||||||||||||||||||||
| Date of first compliant deposit: | 12 October 2022 | |||||||||||||||||||||||||||
| Date of first compliant Open Access: | 12 October 2022 | |||||||||||||||||||||||||||
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