Kharchuk S. The physical characteristics of dust of the selected long-period comets derived from the dynamical modeling

The results of the Monte Carlo model analysis of the dust tails formation of selected comets are presented. Significant role of the dust particles fragmentation in forming dust tail of comet C/1995 O1 (Hale–Bopp) is proved. A new model calculation method of fragmentation process of highly porous comet dust particles is developed. The brightness distribution in the comet dust tail was fitted to similar model parameters for three different dates with taking into account the fragmentation process. The striae dust features in comet tails is investigated. The presence of local active regions on the rotating nucleus surface is suggested as a possible explanation of this phenomenon. The striated features are caused by different dust production rate, depending on the Sun illumination. The effectiveness of the proposed mechanism is confirmed as result of modeling studies. The model experiments evaluate the axial rotation periods of comets C/1910 A1 (Great January Comet), C/1957 P1 (Mrkos), C/1962 C1 (Seki–Lines), C/1975 V1 (West), C/2006 P1 (McNaught), C/2011 L4 (PanSTARRS). Physical characteristics of the dust particles such as sizes, size distribution, ejection velocities, and their lifetimes are received as results of dynamic modeling of the dust tail formation of comets C/1995 O1 (Hale–Bopp), C/2006 P1 (McNaught), C/1910 A1 (Great January Comet), C/1957 P1 (Mrkos), C/1962 C1 (Seki–Lines), C/1975 V1 (West), C/2011 L4 (PanSTARRS), C/2012 S1 (ISON), C/2012 K5 (LINEAR).