H<i>α</i> and He I absorption in HAT-P-32 b observed with CARMENES
S. Czesla, M. Lampón, J. Sanz‐Forcada, A. García Muñoz, M. López‐Puertas, L. Nortmann, Dongdong Yan, E. Nagel, F. Yan, J. H. M. M. Schmitt, J. Aceituno, P. J. Amado, J. A. Caballero, N. Casasayas-Barris, Th. Henning, S. Khalafinejad, Karan Molaverdikhani, D. Montes, Ε. Πάλλη, A. Reiners, P. C. Schneider, I. Ribas, A. Quirrenbach, M. R. Zapatero Osorio, M. Zechmeister
Abstract
We analyze two high-resolution spectral transit time series of the hot Jupiter HAT-P-32 b obtained with the CARMENES spectrograph. Our new XMM-Newton X-ray observations of the system show that the fast-rotating F-type host star exhibits a high X-ray luminosity of 2.3 × 10 29 erg s −1 (5–100 Å), corresponding to a flux of 6.9 × 10 4 erg cm −2 s −1 at the planetary orbit, which results in an energy-limited escape estimate of about 10 13 g s −1 for the planetary mass-loss rate. The spectral time series show significant, time-dependent absorption in the H α and He I λ 10833 triplet lines with maximum depths of about 3.3% and 5.3%. The mid-transit absorption signals in the H α and He I λ 10833 lines are consistent with results from one-dimensional hydrodynamic modeling, which also yields mass-loss rates on the order of 10 13 g s −1 . We observe an early ingress of a redshifted component of the transmission signal, which extends into a redshifted absorption component, persisting until about the middle of the optical transit. While a super-rotating wind can explain redshifted ingress absorption, we find that an up-orbit stream, transporting planetary mass in the direction of the star, also provides a plausible explanation for the pre-transit signal. This makes HAT-P-32 a benchmark system for exploring atmospheric dynamics via transmission spectroscopy.