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We present the values of a ratio β of the solar radiation pressure force to the solar gravity on the finite circular cylindrical grains, as functions of an aspect ratio of the cylinder and an incident angleof the solar radiation. By using the resulting formula of β() , the trajectory of the Kepler orbit for the rotating silicate cylinder is computed associated with a spin motion under the assumption that the spin axis is along the shortest axis of the cylinder and points to the direction perpendicular to the solar radiation. We found for the silicate cylinder grain with a mass equivalent to a sphere with a radius of 0.15 µm, and the aspect ratio of 2.0 that a heliocentric distance of the grain varies periodically with a time, having an amplitude of the fluctuation in the heliocentric distance of about 0.02 AU, where the spin velocity is 0.25 rotation /day and the initial orbit has a semi-major axis 3.0 AU and an eccentricity 0. In addition, during such a fluctuation of the heliocentric distance, the instantaneous eccentricity of the orbit also varies simultaneously from 0 to 1.6 with the rotation of the grain. This implies that the in-situ measurements of orbital elements of impact grains on the dust detector may record those instantaneous orbital elements related to the phase of the grain's rotation. grain, while the solar gravitational force is proportional to its mass. This suggests that the projected-area to mass ratio is a key parameter to understand the dynamical behavior of dust grain in the interplanetary space. If we consider the situation when the projected area to mass ratio changes with the spin motion of the grain, a time variation of β arises, where β is a ratio of the solar radiation force to the solar gravity on the grain. This variation of β would lead to the periodic fluctuation of the Kepler orbit of the grain, associated with its rotational state. It is our motivation to prove this prediction quantitatively.

Orbital variation of the rotating non-spherical dust grains due to change of the solar radiation forces by shape effect