Handbook for photographic meteor observations by Jurgen Rendtel.

By Jurgen Rendtel.

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A longer list is given by Ceplecha (1966) and Ceplecha (1971). Table 3-7: List of spectral lines frequently found in meteor spectra and their relative intensities. The identification of the lines (numbers) in our example is also given. Lines marked with an asterisk appear bright in spectra of fast meteors, such as the Perseids, but much fainter in spectra of slow meteors. 5 Fe 3 ident. 9 H 2* ident. number 48 IMO Photographic Handbook Another way to relate measured coordinates x of dispersion into wavelengths λ is through the use of an interpolation polynomial, especially for gratings.

These appear bright against the night sky. However, much mystery still surrounds the physics of train phenomena (Ceplecha, 1991). A large meteoroid entering the atmosphere also distributes a substantial amount of material along its trajectory as it ablates. This may lead to the formation of the so-called smoke trains, which do not emit light, and are composed of dust particles. Both types of trains occur at altitudes above 20 km. At these heights strong winds exist that will cause the trains to distort within a short period after formation.

The amount of dispersion as a function of the wavelength. This has to be done for a given combination of lens and dispersing element (prism or grating). For this, we need an object in the same field providing well defined lines of known wavelength. Such a source can be either a suitable reference star, preferably one of type A, or a terrestrial emission lamp providing enough lines in different parts of the spectrum. For example, a mercury-vapour-lamp, which may be in use for street illumination, will suit this purpose (Fig.

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