HAT-P-11 Spectral Energy Distribution

Description: Spectral energy distribution (SED) ascii file related to Nature-Astronomy paper by Ben-Jaffel et al., 2021:




HAT-P-11-stellar-spectrum-1AU-REG.datDownload 1.8 MB

Ascii file that contains HAT-P-11's spectral energy distribution (SED) at 1 AU from the star. The SED is sampled at a regular 1 Angstrom wavelength bin. See full description in Ben-Jaffel et al., Nature Astronomy, 2021

Citation: Signatures of Strong Magnetization and Metal-poor Atmosphere for a Neptune-Size Exoplanet, Ben-Jaffel et al. 2021, available here
Author:L. Ben-Jaffel, G. Ballester, A. Garcia-Munoz, P. Lavvas, et al.
Title:Signatures of Strong Magnetization and Metal-poor Atmosphere for a Neptune-Size Exoplanet
Reference of the paper linked to this data:Ben-Jaffel et al, 2021, Nature Astronomy, in press.
Ressource type:Ascii files

Abstract of the paper :

No exoplanetary magnetosphere has been unambiguously detected. Investigations of star-planet interaction and neutral atomic hydrogen absorption during transit to detect magnetic fields in hot Jupiters have been inconclusive, and interpretations of the transit absorption non-unique. In contrast, ionized species escaping a magnetized exoplanet, particularly from the polar caps, should populate the magnetosphere, allowing detection of different regions from the plasmasphere to the extended magnetotail, and characterization of the magnetic field producing them. Here, we report ultraviolet observations of HAT-P-11b, a low-mass (0.08 MJ) exoplanet showing strong, phase-extended transit absorption of neutral hydrogen (maximum and tail transit depths of 32 +/- 4%, 27 +/- 4%) and singly ionized carbon (15 +/- 4%, 12.5 +/- 4%). We show that the atmosphere should have less than six times the solar metallicity (at 200 bars), and the exoplanet must also have an extended magnetotail (1.8–3.1 AU). The HAT-P-11b equatorial magnetic field strength should be about 1–5 Gauss. Our panchromatic approach using ionized species to simultaneously derive metallicity and magnetic field strength can now constrain interior and dynamo models of exoplanets, with implications for formation and evolution scenarios.

Institut Astrophysique de Paris, CNRS, Sorbonne Université,
Lunar & Planetary Laboratory, Tucson (USA),
AIM, CEA, CNRS, Université Paris-Saclay, Université de Paris,
Groupe de Spectroscopie Moléculaire et Atmosphérique, Université de Reims, Champagne-Ardenne,
Department of Earth & Planetary Sciences, John Hopkins University, Baltimore (USA),
Centro de Astrobiología (CSIC-INTA), ESAC, Madrid (Spain),
Lowell Center for Space Science and Technology, University of Massachusetts, Lowell (USA)
NASA Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena (USA),
Center of Excellence in Information Systems, Tennessee State University, Nashville (USA)
DTU Space, National Space Institute, Technical University of Denmark, Lyngby (Denmark),
Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge (USA),
School of Physics, University of Bristol, HH Wills Physics Laboratory, Bristol (UK),
Center for Astrophysics, Harvard & Smithsonian, Cambridge (USA)