The work is devoted to the study of gyroscopic phenomena in the interaction of a rotating fullerene molecule and a xenon atom incident on it. The methods of classical molecular physics are used: intermolecular potentials, Newton's equations for describing the motion of particles, and the Runge–Kutta numerical method of high order of accuracy. A mathematical model is constructed and implemented for the rotation frequencies of fullerene up to 1014 Hz and the speed of the incident xenon atom of the order of 103 m s−1. For such parameters of the problem, the de Broglie wavelength of the incident atom and the fullerene molecule become smaller than the diameter of the carbon atomic nucleus. This made it possible to apply the Newtonian approach without involving quantum mechanics. The aim of this work is the consistent application of the apparatus of classical mechanics to reveal the effect of the precession of rotating fullerene inside fullerite.
I present high-resolution column density maps of two molecular clouds (MCs) having strikingly different star formation rates. To better understand the unusual, massive G216-2.5, an MC with no massive star formation, the distribution of its molecular gas is compared to that of the Rosette MC. Far-infrared data from Herschel are used to derive N(H 2 ) maps of each cloud and are combined with I CO data to determine the CO-to-H 2 ratio, X CO . In addition, the probability distribution functions (PDFs) and cumulative mass fractions of the clouds are compared. For G216-2.5, á ñ =Ń (H ) 7.8 10 2 20 cm −2 and á ñ =X 2.2 10 CO 20 cm −2 (K km s −1 ) −1 ; for the Rosette, á ñ =Ń (H ) 1.8 10 2 21 cm −2 and á ñ =X 2.8 10 CO 20 cm −2 (K km s −1 ) −1 . The PDFs of both clouds are lognormal for extinctions below ∼2 mag and both show departures from log-normality at high extinctions. Although it is the less-massive cloud, the Rosette has a higher fraction of its mass in the form of dense gas and contains M 1389 of gas above the so-called extinction threshold for star formation, = A 7.3 V mag. The G216-2.5 cloud has M 874of dense gas above this threshold.
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