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Star-planet interaction through spectral lines

Published online by Cambridge University Press:  24 September 2020

C. Villarreal D’Angelo Open the ORCID record for C. Villarreal D’Angelo [Opens in a new window] ,
A. A. Vidotto Open the ORCID record for A. A. Vidotto [Opens in a new window] ,
A. Esquivel ,
M. A. Sgró ,
T. Koskinen  and
L. Fossati
C. Villarreal D’Angelo
Affiliation:
School of Physics, Trinity College Dublin, The University of Dublin College Green, Dublin 2, Dublin, Ireland email: villarrc@tcd.ie
A. A. Vidotto
Affiliation:
School of Physics, Trinity College Dublin, The University of Dublin College Green, Dublin 2, Dublin, Ireland email: villarrc@tcd.ie
A. Esquivel
Affiliation:
Instituto de Ciencias Nucleares, UNAM, Ciudad de México, México Instituto de Astronomía Teórica y Experimental, Conicet-UNC, Córdoba, Argentina
M. A. Sgró
Affiliation:
Instituto de Astronomía Teórica y Experimental, Conicet-UNC, Córdoba, Argentina
T. Koskinen
Affiliation:
University of Arizona, Lunar and Planetary Laboratory, Tucson, Arizona, United States
L. Fossati
Affiliation:
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
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Abstract

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The growth of spectroscopic observations of exoplanetary systems allows the possibility of testing theoretical models and studying the interaction that exoplanetary atmospheres have with the wind and the energetic photons from the star. In this work, we present a set of numerical 3D simulations of HD 209458b for which spectral lines observations of their evaporative atmosphere are available. The different simulations aim to reproduce different scenarios for the star-planet interaction. With our models, we reconstruct the Lyα line during transit and compare with observations. The results allows us to analyse the shape of the line profile under these different scenarios and the comparison with the observations suggest that HD209458b may have a magnetic field off less than 1 G. We also explore the behaviour of the magnesium lines for models with and without magnetic fields.

Keywords

stars: individualHD209458stars: planetary systemsstars: windsoutflowsline: profilesmagnetic fieldsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 280 - 285
Copyright
© International Astronomical Union 2020

References

Bourrier, V., Lecavelier des Etangs, A., & Vidal-Madjar, A. 2014, A&A, 565, A105 Google Scholar
Esquivel, A., Schneiter, M., Villarreal D’Angelo, C., Sgró, M. A., et al. 2019, MNRAS, 487, 5788 CrossRefGoogle Scholar
Murray-Clay, R. A., Chiang, E. I., & Murray, N. 2009, ApJ, 693, 23 CrossRefGoogle Scholar
Linsky, J. L., Yang, H., France, K., et al. 2010, ApJ, 717, 1291 CrossRefGoogle Scholar
Torres, G., Winn, J. N., & Holman, M. J. 2008, ApJ, 677, 1324 CrossRefGoogle Scholar
Sanz-Forcada, J., Micela, G., Ribas, I., et al. 2011, A&A, 532, A6 Google Scholar
Vidal-Madjar, A., Lecavelier des Etangs, A., Désert, J.-M., et al. 2003, Nature, 422, 143 CrossRefGoogle Scholar
Vidal-Madjar, A., Désert, J.-M., Lecavelier des Etangs, A., et al. 2004, ApJ, 604, L69 CrossRefGoogle Scholar
Vidal-Madjar, A., Huitson, C. M., Bourrier, V., et al. 2013, A&A, 560, A54 Google Scholar
Villarreal D’Angelo, C., Schneiter, M., Costa, A., et al. 2014, MNRAS, 438, 1654 CrossRefGoogle Scholar
Villarreal D’Angelo, C., Esquivel, A., Schneiter, M., M., Sgró, M. A. 2018, MNRAS, 479, 3115 CrossRefGoogle Scholar