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Photometric observations of comet C/1995 O1 (Hale–Bopp)) carried out at the Stará Lesná Observatory since February to April 1997 are analyzed and discussed. Emission band fluxes and continuum fluxes are presented, from which the total numbers of molecules in the columns of the coma encircled by diaphragms are calculated. The production rates are estimated from the conventional Haser model. We found that the photometric exponent of dust contribution two months prior perihelion was n = 5.2. The photometric exponent n of the cometary magnitude solely to the C2emission alone equals 3.3 and that of CN equals 2.5. These values can be explained by a fact that the maximums of production rates of the gases were reached between March 2 and 12 and not at the perihelion as it is valid for dust.These results are compared with the values of 1P/Halley (1986 III)) under the similar conditions, obtained with the same method and instrument. C/Hale–Bopp exhibited 4.1 times more molecules radiating the CN-emission than 1P/Halley in the same column of the coma. The continuum flux of C/Hale–Bopp was also very strong. The ratios (to 1P/Halley)) are 94:1 (Cont. 484.5)) and 74:1 (Cont. 365.0)). The cometary colour was the same as that of the Sun.

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