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The GAPS Programme at TNG. XXXII. The revealing non-detection of metastable HeI in the atmosphere of the hot Jupiter WASP-80b by Fossati, L.; Guilluy, G.; Shaikhislamov, I. F.; Carleo, I.; Borsa, F.; Bonomo, A. S.; Giacobbe, P.; Rainer, M.; Cecchi-Pestellini, C.; Khodachenko, M. L.; Efimov, M. A.; Rumenskikh, M. S.; Miroshnichenko, I. B.; Berezutsky, A. G.; Nascimbeni, V.; Brogi, M.; Lanza, A. F.; Mancini, L.; Affer, L.; Benatti, S.; Biazzo, K.; Bignamini, A.; Carosati, D.; Claudi, R.; Cosentino, R.; Covino, E.; Desidera, S.; Fiorenzano, A.; Harutyunyan, A.; Maggio, A.; Malavolta, L.; Maldonado, J.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Piotto, G.; Poretti, E.; Scandariato, G.; Sozzetti, A.; Stoev, H. is a scholarly article available to read on EtoBox.

What is The GAPS Programme at TNG. XXXII. The revealing non-detection of metastable HeI in the atmosphere of the hot Jupiter WASP-80b about?

The hot Jupiter WASP-80b has been identified as a possible excellent target for detecting and measuring HeI absorption in the upper atmosphere. We observed 4 primary transits of WASP-80b in the optical and near-IR using the HARPS-N and GIANO-B high-resolution spectrographs, focusing on the HeI triplet. We further employed a three-dimensional hydrodynamic aeronomy model to understand the observational results. We did not find any signature of planetary absorption at the position of the HeI triplet with an upper limit of 0.7% (i.e. 1.11 planetary radii; 95% confidence level). We re-estimated the stellar high-energy emission that we combined with a stellar photospheric model to generate the input for the hydrodynamic modelling. We obtained that, assuming a solar He to H abundance ratio, HeI absorption should have been detected. Considering a stellar wind 25 times weaker than solar, we could reproduce the non-detection only assuming a He to H abundance ratio about 16 times smaller than solar. Instead, considering a stellar wind 10 times stronger than solar, we could reproduce the non-detection only with a He to H abundance ratio about 10 times smaller than solar. We attempted to unders

Author

Fossati, L.; Guilluy, G.; Shaikhislamov, I. F.; Carleo, I.; Borsa, F.; Bonomo, A. S.; Giacobbe, P.; Rainer, M.; Cecchi-Pestellini, C.; Khodachenko, M. L.; Efimov, M. A.; Rumenskikh, M. S.; Miroshnichenko, I. B.; Berezutsky, A. G.; Nascimbeni, V.; Brogi, M.; Lanza, A. F.; Mancini, L.; Affer, L.; Benatti, S.; Biazzo, K.; Bignamini, A.; Carosati, D.; Claudi, R.; Cosentino, R.; Covino, E.; Desidera, S.; Fiorenzano, A.; Harutyunyan, A.; Maggio, A.; Malavolta, L.; Maldonado, J.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Piotto, G.; Poretti, E.; Scandariato, G.; Sozzetti, A.; Stoev, H.

Published

2021

Language

EN