The solar wind-comet interaction, one of the basic processes investigated in the cometary physics, may be judged by the ion's behavior. CO is one of the most abundant cometary atmosphere species. A synthetic spectrum of CO was created to analyze Halley's comet spectra. The values of some molecular constants were specified in order to improve the accuracy of the computations. It was established that the more appropriate value of the spin-rotational interaction parameter y for the B2 state is 0.0192. The use of different values of y for the higher vibrational levels (v>O) of the X and B states didn't help for a more precise result. That's why it is recommended to use the same value y for all vibrational levels of a given state. The value -122.0 was determined for the spin-orbital interaction parameter A of the A2'it state. The molecular model, needed to create a spectrum which adequately reproduces the total CO glow has been specified: v0÷4 for X2E state, v=O÷6 for A2ir state, '=O÷2 for B2E state and rotational levels up to N=12 for an optimal theoretical spectrum and up to N=8 for analysis of Halley's comet spectra registered by the three-channel spectrometer on board the Vega-2.
Spectra in the visible region measured on board the Vega-2 station are analysed to obtain the solar spectrum continuum reflected by the dust particles in the Halley comet coma. It is suggested to determine the continuum level for every individual spectrum. By the time of Vega encounter, the concentration and distribution of particles around the comet had changed. This resulted in a different spectral indices for spectra measured in different time. The cumulative size index has been calculated for each specific spectrum by linear regression on the basis of a random number of dust points. Eleven dust continuum wavelengths are selected. The spectral index shows the mean particle size in the line of sight column around the nucleus (values calculated for 1019 spectra are in the interval of 2.85 -3.48) . Its change with the radial distance to the nucleus is discussed. The continuum spectra are calculated with the obtained values of the spectral index and are normalised to the real spectra on the minimum of interval of pixels in relation to the specific dust intensity, with the help of a linear regression. The continuum spectrum follows well the course of the specific Halley's comet spectrum.
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