The Dust Tail of Comet Bradfield 1987XXIX
In this paper the reduction and the analysis of two images comcerning the dust tail of Comet Bradfield 1987XXIX are discussed. The plates (CRT7 + W16) were obtained by means of a 20/25/50 cm Schmidt camera. The adopted emulsion and filter combination (pass band 520–570 nm) approximates the standard V photometric system, thus dropping most of the plasma emissions, being sensitive only to neutral emissions in the inner coma due to C2. We use SAO and GSPC-I calibration stars to measure the sky brightness, which resulted V = 20.0 ± 0.3 mag arcsec-2. To these data we apply the inverse numerical method (Fulle, 1989) which gives information about the dust loss rates, the dust ejection velocity from the inner coma and the size distribution. We consider grains of diameters between 1 µm and 1 cm ejected during the time interval -280 < t < +40 (days related to perihelion). The total mass ejected during mis time interval is (4 ± 1) 1014 g (for an albedo Ap(α) = 0.03), higher than that of Comet Kohoutek 1973XII, and the mass of meteoroids injected into bound orbits is (2 ± 1) 1014 g. The power index of the time-averaged size distribution is - 3.2 ± 0.2.
KeywordsMass Loss Rate Power Index Interplanetary Dust Filter Combination Short Period Comet
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