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Radiation chemistry in astrochemical models: From the laboratory to the ISM

Published online by Cambridge University Press:  12 October 2020

Christopher N. Shingledecker Open the ORCID record for Christopher N. Shingledecker [Opens in a new window] ,
Alexei Ivlev ,
Johannes Kästner ,
Eric Herbst  and
Paola Caselli
Christopher N. Shingledecker
Affiliation:
Zentrum für astrochemische Studien, Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching bei München, Germany emails: [email protected], [email protected], [email protected] Institute for Theoretical Chemistry, University of Stuttgart, Pfaffenwaldring 55, 70569 Stuttgart, Germany email: [email protected]
Alexei Ivlev
Affiliation:
Zentrum für astrochemische Studien, Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching bei München, Germany emails: [email protected], [email protected], [email protected]
Johannes Kästner
Affiliation:
Institute for Theoretical Chemistry, University of Stuttgart, Pfaffenwaldring 55, 70569 Stuttgart, Germany email: [email protected]
Eric Herbst
Affiliation:
Department of Chemistry, University of Virginia, McCormick Road, PO Box 400319, Charlottesville, VA 22904, USA email: [email protected] Department of Astronomy, University of Virginia, 530 McCormick Rd, Charlottesville, VA 22904, USA
Paola Caselli
Affiliation:
Zentrum für astrochemische Studien, Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching bei München, Germany emails: [email protected], [email protected], [email protected]
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Abstract

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Most interstellar and planetary environments are suffused by a continuous flux of several types of ionizing radiation, including cosmic rays, stellar winds, x-rays, and gamma-rays from radionuclide decay. There is now a large body of experimental work showing that these kinds of radiation can trigger significant physicochemical changes in ices, including the dissociation of species (radiolysis), sputtering of surface species, and ice heating. Even so, modeling the chemical effects that result from interactions between ionizing radiation and interstellar dust grain ice mantles has proven challenging due to the complexity and variety of the underlying physical processes. To address this shortcoming, we have developed a method whereby such effects could easily be included in standard rate-equations-based astrochemical models. Here, we describe how such models, thus improved, can fruitfully be used to simulate experiments in order to better understand bulk chemistry at low temperatures.

Keywords

astrochemistryatomic processesdiffusioncomets: generalISM: cosmic raysISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 454 - 455
Copyright
© International Astronomical Union 2020

References

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