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X-ray photodesorption from water ice in protoplanetary disks and X-ray-dominated regions

Nature Astronomyvolume 2pages796801 (2018) | Download Citation

Abstract

Water is the main constituent of interstellar ices, and it plays a key role in the evolution of many regions of the interstellar medium, from molecular clouds to planet-forming disks1. In cold regions of the interstellar medium, water is expected to be completely frozen out onto the dust grains. Nonetheless, observations indicate the presence of cold water vapour, implying that non-thermal desorption mechanisms are at play. Photodesorption by ultraviolet photons has been proposed to explain these observations2,3, with the support of extensive experimental and theoretical work on ice analogues4,5,6. In contrast, photodesorption by X-rays, another viable mechanism, has been little studied. The potential of this process to desorb key molecules such as water, intact rather than fragmented or ionized, remains unexplored. We experimentally investigated X-ray photodesorption from water ice, monitoring all desorbing species. We found that desorption of neutral water is efficient, while ion desorption is minor. We derived yields that can be implemented in astrochemical models. These results open up the possibility of taking into account the X-ray photodesorption process in the modelling of protoplanetary disks or X-ray-dominated regions.

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Acknowledgements

We thank C. Walsh for insights on X-rays in protoplanetary disks, D. Lis for comments on the paper and P. Marie-Jeanne for technical support. We acknowledge SOLEIL for the provision of synchrotron radiation facilities under project 20161406, and we thank N. Jaouen and the SEXTANTS team for their help on the beamline. This work was supported by the Programme National ‘Physique et Chimie du Milieu Interstellaire’ (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES. Financial support from LabEx MiChem, part of the French state funds managed by the ANR within the investissements d’avenir programme under reference ANR-11-10EX-0004-02, and by the Ile-de-France region DIM ACAV programme, is gratefully acknowledged. This work was done in collaboration with and through financial support from the European Organization for Nuclear Research (CERN) under collaboration agreement KE3324/TE.

Author information

Affiliations

  1. LERMA, Sorbonne Université, Observatoire de Paris, Université PSL, CNRS, Paris, France

    • R. Dupuy
    • , M. Bertin
    • , G. Féraud
    • , M. Hassenfratz
    • , X. Michaut
    • , T. Putaud
    • , L. Philippe
    • , P. Jeseck
    •  & J.-H. Fillion
  2. Laboratori Nazionali di Frascati, INFN, Frascati, Italy

    • M. Angelucci
    •  & R. Cimino
  3. CERN, Geneva, Switzerland

    • V. Baglin
  4. Laboratoire de Chimie Physique, CNRS, Univ. Paris-Sud, Université Paris-Saclay, Orsay, France

    • C. Romanzin

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Contributions

R.D. treated and analysed the data and wrote the manuscript. M.B., G.F., M.H. and J.-H.F. provided extensive input on the data analysis and the manuscript. J.-H.F., M.B., G.F. and R.D. initiated and supervised the project. J.-H.F., M.B. and P.J. designed the experimental set-up. G.F. contributed to the bibliographic work. All authors participated in the experimental runs at the SOLEIL synchrotron where the data were acquired.

Competing interests

The authors declare no competing interests.

Corresponding author

Correspondence to R. Dupuy.

Supplementary information

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    Supplementary Text, Supplementary Figures 1–6, Supplementary References

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DOI

https://doi.org/10.1038/s41550-018-0532-y