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The origin of hydrogen around HD 209458b

Author

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  • A. Lecavelier des Etangs

    (* CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France
    † UPMC Université Paris 6, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France. lecaveli@iap.fr)

  • A. Vidal-Madjar

    (* CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France
    † UPMC Université Paris 6, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France. lecaveli@iap.fr)

  • J.-M. Désert

    (* CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France
    † UPMC Université Paris 6, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France. lecaveli@iap.fr)

Abstract

Arising from: M. Holmström et al. Nature 451, 970–972 (2008)10.1038/nature06600 ; Holmström et al. reply Using numerical simulation, Holmström et al.1 proposed a plausible alternative explanation of the observed Lyman-α absorption that was seen during the transit of HD 209458b (ref. 2). They conclude that radiation pressure alone cannot explain the observations and that a peculiar stellar wind is needed. Here we show that radiation pressure alone can in fact produce the observed high-velocity hydrogen atoms. We also emphasize that even if the stellar wind is responsible for the observed hydrogen, to have a sufficient number of atoms for charge exchange with stellar wind, the energetic neutral atom (ENA) model also needs a significant escape from the planet atmosphere of similar amplitude as quoted in ref. 2.

Suggested Citation

  • A. Lecavelier des Etangs & A. Vidal-Madjar & J.-M. Désert, 2008. "The origin of hydrogen around HD 209458b," Nature, Nature, vol. 456(7219), pages 1-1, November.
    • Handle: RePEc:nat:nature:v:456:y:2008:i:7219:d:10.1038_nature07402
    DOI: 10.1038/nature07402
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