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On inelastic hydrogen atom collisions in stellar atmospheres
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics.
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics.
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2011 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 530, A94- p.Article in journal (Refereed) Published
Abstract [en]

The influence of inelastic hydrogen atom collisions on non-LTE spectral line formation has been, and remains to be, a significant source of uncertainty for stellar abundance analyses, due to the difficulty in obtaining accurate data for low-energy atomic collisions either experimentally or theoretically. For lack of a better alternative, the classical "Drawin formula" is often used. Over recent decades, our understanding of these collisions has improved markedly, predominantly through a number of detailed quantum mechanical calculations. In this paper, the Drawin formula is compared with the quantum mechanical calculations both in terms of the underlying physics and the resulting rate coefficients. It is shown that the Drawin formula does not contain the essential physics behind direct excitation by H atom collisions, the important physical mechanism being quantum mechanical in character. Quantitatively, the Drawin formula compares poorly with the results of the available quantum mechanical calculations, usually significantly overestimating the collision rates by amounts that vary markedly between transitions.

Place, publisher, year, edition, pages
2011. Vol. 530, A94- p.
Keyword [en]
atomic data, line: formation, stars: abundances, stars: atmospheres
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:uu:diva-154956DOI: 10.1051/0004-6361/201116745ISI: 000291027400094OAI: oai:DiVA.org:uu-154956DiVA: diva2:422801
Available from: 2011-06-14 Created: 2011-06-14 Last updated: 2017-12-11Bibliographically approved

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Barklem, Paul

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