On the meteor trail spectra
- Shafiev, R. I.
- Aug 1, 1987.
- Physical Description:
- 1 electronic document
- Additional Creators:
- Mukhamednazarov, S., Maltsev, N. V., and Ovezgeldyev, O. G.
- hdl.handle.net , Connect to this object online.
- Restrictions on Access:
- Unclassified, Unlimited, Publicly available.
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- Meteor radiation appears as a result of collisions between meteoroid atoms and air molecules. Depending on duration, this radiation is usually divided into the following types: radiation of the meteor head; radiation of a coma surrounding or immediately following the meteor head; radiation of a trail formed as a result of fragments lagging behind or by the afterglow; and radiation of a meteor train forming from a tail as a result of various chemical and dynamical processes. To investigate physical processes caused by each of the above types, it is necessary to obtain the corresponding experimental data. The physical processes of the radiation and the measurement of the experimental data is discussed.
- Other Subject(s):
- NASA Technical Reports Server (NTRS) Collection.
- Document ID: 19880005151.
Accession ID: 88N14533.
International Council of Scientific Unions, Middle Atmosphere Program. Handbook for MAP, Volume 25; p 222-227.
- No Copyright.
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