Hostname: page-component-848d4c4894-r5zm4 Total loading time: 0 Render date: 2024-07-07T14:04:49.187Z Has data issue: false hasContentIssue false
  • English
  • Français

Chemical Composition of an Emanation from Comets: Identification of the 3 Micron Comet Feature

Published online by Cambridge University Press:  12 April 2016

A. Sakata ,
S. Wada  and
A.T. Tokunaga
A. Sakata
Affiliation:
Dept. of Applied Phys. and Chem., University of Electro-Communications, Chofugaoka, Choin, Tokyo 182, Japan
S. Wada
Affiliation:
Dept. of Chemistry, University of Electro-Communications, Chofugaoka, Chofu, Tokyo 182, Japan
A.T. Tokunaga
Affiliation:
Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, HI 96822U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Recent high resolution observations of comets revealed a detailed spectral shape of the 3.4 μ feature. We measured IR spectra of simple 14 hydrocarbon molecules and made ”synthesized comet spectrum”. Peak wavelength and spectral shape of the synthesized spectrum are well in agreement with the observed comet features.

Type
Cometary Dust: Observations and Evolution
Information
International Astronomical Union Colloquium , Volume 126: Origin and Evolution of Interplanetary Dust , 1991 , pp. 241 - 244
Copyright
Copyright © Kluwer 1991

References

Brooke, T.Y., and Tokunaga, A.T. (1990) ’ Detection of the 3.4 μm emission feature in comets Brorsen-Metcalf and Okazaki-Levy-Rudenko (1989r) and an observational summary’, submitted to A. J.CrossRefGoogle Scholar
Knacke, R.F., Brooke, T.Y., and Joyce, R.R. (1986) ’Observations of 3.2-3.6 micron emission features in comet Halleyd’, Ap. J. 310, L49–L53.Google Scholar