Hα and He I absorption in HAT-P-32 b observed with CARMENES Detection of Roche lobe overflow and mass loss
| Autor: | S. Czesla, M. Lampón, J. Sanz-Forcada, A. García Muñoz, M. López-Puertas, L. Nortmann, D. 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, K. Molaverdikhani, D. Montes, E. Pallé, A. Reiners, P. C. Schneider, I. Ribas, A. Quirrenbach, M. R. Zapatero Osorio, M. Zechmeister |
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| Přispěvatelé: | European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Natural Science Foundation of China, German Research Foundation |
| Rok vydání: | 2021 |
| Předmět: |
Physics
Astrofísica Astrophysics::High Energy Astrophysical Phenomena individual: HAT-P-32 [Planets and satellites] Techniques: spectroscopic Astronomy and Astrophysics X-rays: stars Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics spectroscopic [Techniques] Space and Planetary Science atmospheres [Planets and satellites] Planets and satellites: individual: HAT-P-32 Planets and satellites: atmospheres Roche lobe Astrophysics::Earth and Planetary Astrophysics Absorption (electromagnetic radiation) stars [X-rays] Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | E-Prints Complutense. Archivo Institucional de la UCM instname Digital.CSIC. Repositorio Institucional del CSIC |
| Popis: | 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 Hα and Hea Iλ10833 triplet lines with maximum depths of about 3.3% and 5.3%. The mid-transit absorption signals in the Hα and Hea Iλ10833 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. © ESO 2021. CARMENES is an instrument for the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisica de Andalucia (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Cientificas (CSIC), the Ministerio de Economia y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the MINECO, the Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme and Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of BadenWurttemberg and Niedersachsen, and by the Junta de Andalucia. Based on data from the CARMENES data archive at CAB (CSIC-INTA). We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the ERDF through projects PID2019-109522GB-C5[1:4]/AEI/10.13039/501100011033 PGC2018-098153-B-C33 and the Centre of Excellence "Severo Ochoa" and "Maria de Maeztu" awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM-2017-0737), the Generalitat de Catalunya/CERCA programme. D. Yan acknowledges support by the Strategic Priority Research Program of Chinese Academy of Sciences, Grant No. XDB 41000000 and National Natural Science Foundation of China (Nos. 11973082). SC and EN acknowledge DFG support under grants CZ 222/3-1 and CZ 222/5-1. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. |
| Databáze: | OpenAIRE |
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