An approach to the problem of a meteoric complex called the Interaction Meteor Complex (IMG) is applied and discussed, where author^s former idea of the interaction layer (Rajchl 1969) is generalized. The role of an extended interaction of meteoroids is ephasized, both with planet surfaces and/or their satellites and with planet atmospheres, elastic or inelastic in form. The dissipation and related formative aspect are joined in one complex and compared with a topological compact. Examples of all the above mentioned types of interaction are presented. In more detail the
inelastic interaction with the Earth atmosphere of whole "spectrum" from faint meteors detected by TV technique to Fireball Network bolides, is considered. First results in the form of a ψ structure and cross-complementarity are reported. The possibility of the existence of another "enlarged" ψ structure is anticipated from topological
aspects and supported for the outer planets of the Solar Planetary System by results of Levin and Simonenko (1982).
Nine objective prism spectrograms by means of two cameras were achieved. It was impossible to point directly at the comet image by using the larger camera. The motions in α of both the camera and the comet were the same. The motion difference in δ was determined experimentally and introduced as correction. The photometrical tracings of the comet head and tail and of the stars were made by using a recording microphotometer. The computed dispersion curve was corrected by using the main comet head emissions. The identification of the emissions was done by a comparison with [2] and [3]. The spectrograms show strong CN and Na emissions. It was assumed, that the background below the emissions was due to continuous spectrum. Then its amplitude is nearly twice that of the emission lines. The amplitude ratio continuum/emission in the tail was 1 : 0·6. The spectrograms from the end of May show only weak C2 emissions. The tail directied towards the Sun was unobservable during our observations.
The study of one spectrum of comet Mrkos obtained on 1957 August 23 with an objective prism of dispersion 52 A/mm for λ 4000 A is given in this paper. and Článek doplňuje list se snímky komety (nestránkováno)