Abstract
A long-lived (>32 min) persistent meteor train has been observed with a low light television camera which was sensitive only to radiation between wavelengths of 700 and 900 nm. The peak emission from the train was about 2 × 1017 photons s−1 m−1 and the meteor which produced the train had a magnitude corrected to the zenith of about −6. It is suggested here that this IR emission arises from the excitation of the atmospheric band of molecular oxygen (b1Σg→X3Σg) by the sodium catalytic process, a process which Baggaley1–3 has previously proposed to be responsible for the visible radiation from persistent meteor trains.
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References
Baggaley, W. J. Bull. astr. Insts Csl. 27, 244–246 (1976).
Baggaley, W. J. Nature 257, 567–568 (1975).
Baggaley, W. J. The Observatory 98, 8–11 (1978).
Lovell, A. C. B. Meteor Astronomy, 131 (Oxford University Press, 1954).
Colin, L. & Myers, M. A. Computed Times of Sunrise and Sunset in the Ionosphere (NASA TM X-1233, 1966).
Chapman, S. in The Aurora and Airglow (eds Armstrong, E. B. & Dalgarno, A.) 204–205 (Pergamon, Oxford, 1955).
Chapman, S. J. geophys. Res. 64, 2064–2065 (1959).
Kolb, C. E. & Elgin, J. B. Nature 263, 488–490 (1976).
Zipf, E. C. Can. J. Chem. 47, 1863–1870 (1969).
Baggaley, W. J. Bull. astr. Insts Csl. 28, 356–359 (1977).
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Hapgood, M. IR observation of a persistent meteor train. Nature 286, 582–583 (1980). https://doi.org/10.1038/286582a0
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DOI: https://doi.org/10.1038/286582a0
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