Wind of change: retrieving exoplanet atmospheric winds from high-resolution spectroscopy
Journal
Date Issued
2020
Author(s)
Seidel, J. V.
•
Ehrenreich, D.
•
•
Bourrier, V.
•
Lavie, B.
•
Allart, R.
•
Wyttenbach, A.
•
Lovis, C.
Abstract
Context. The atmosphere of exoplanets has been studied extensively in recent years, making use of numerical models to retrieve chemical composition, dynamical circulation, or temperature from the data. One of the best observational probes in transmission is the sodium doublet thanks to its extensive cross-section. However, modelling the shape of planetary sodium lines has proven to be challenging. Models with different assumptions regarding the atmosphere have been employed to fit the lines in the literature, yet statistically-sound, direct comparisons of different models are needed to paint a clear picture.
Aims: We aim to compare different wind and temperature patterns, as well as to provide a tool to distinguish them based on their best fit for the sodium transmission spectrum of the hot Jupiter HD 189733b. We parametrise different possible wind patterns that have already been tested the in literature and introduce the new option of an upwards-driven vertical wind.
Methods: We construct a forward model where the wind speed, wind geometry, and temperature are injected into the calculation of the transmission spectrum. We embed this forward model in a nested sampling retrieval code to rank the models via their Bayesian evidence.
Results: We retrieve a best-fit to the HD 189733b data for vertical upward winds |vver(mean)| = 40 ± 4 km s-1 at altitudes above 10-6 bar. With the current data from HARPS, we cannot distinguish wind patterns for higher-pressure atmospheric layers.
Conclusions: We show that vertical upwards winds in the upper atmosphere provide a possible explanation for the broad sodium signature in hot Jupiters. We highlight other influences on the width of the doublet and we explore strong magnetic fields acting on the lower atmosphere as one possible origin of the retrieved wind speed.
Aims: We aim to compare different wind and temperature patterns, as well as to provide a tool to distinguish them based on their best fit for the sodium transmission spectrum of the hot Jupiter HD 189733b. We parametrise different possible wind patterns that have already been tested the in literature and introduce the new option of an upwards-driven vertical wind.
Methods: We construct a forward model where the wind speed, wind geometry, and temperature are injected into the calculation of the transmission spectrum. We embed this forward model in a nested sampling retrieval code to rank the models via their Bayesian evidence.
Results: We retrieve a best-fit to the HD 189733b data for vertical upward winds |vver(mean)| = 40 ± 4 km s-1 at altitudes above 10-6 bar. With the current data from HARPS, we cannot distinguish wind patterns for higher-pressure atmospheric layers.
Conclusions: We show that vertical upwards winds in the upper atmosphere provide a possible explanation for the broad sodium signature in hot Jupiters. We highlight other influences on the width of the doublet and we explore strong magnetic fields acting on the lower atmosphere as one possible origin of the retrieved wind speed.
Volume
633
Start page
A86
Issn Identifier
0004-6361
Ads BibCode
2020A&A...633A..86S
Rights
open.access
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