7 research outputs found
Orbital evolution under action of fast interstellar gas flow
Orbital evolution of an interplanetary dust particle under action of an
interstellar gas flow is investigated. Secular time derivatives of the particle
orbital elements, for arbitrary orbit orientation, are presented. An important
result concerns secular evolution of semi-major axis. Secular semi-major axis
of the particle on a bound orbit decreases under the action of fast
interstellar gas flow. Possible types of evolution of other Keplerian orbital
elements are discussed. The paper compares influences of the Poynting-Robertson
effect, the radial solar wind and the interstellar gas flow on dynamics of the
dust particle in outer planetary region of the Solar System and beyond it, up
to 100 AU.
Evolution of putative dust ring in the zone of the Edgeworth-Kuiper belt is
studied. Also non-radial solar wind and gravitational effect of major planets
may play an important role. Low inclination orbits of micron-sized dust
particles in the belt are not stable due to fast increase of eccentricity
caused by the interstellar gas flow and subsequent planetary perturbations -
the increase of eccentricity leads to planet crossing orbits of the particles.
Gravitational and non-gravitational effects are treated in a way which fully
respects physics. As a consequence, some of the published results turned out to
be incorrect. Moreover, the paper treats the problem in a more general way than
it has been presented up to now.
The influence of the fast interstellar neutral gas flow might not be ignored
in modeling of evolution of dust particles beyond planets.Comment: 12 pages, 7 figure
The non-radial component of the solar wind and motion of dust near mean motion resonances with planets
We investigate the effect of solar wind and solar electromagnetic radiation on
the dynamics of spherical cosmic dust particles. We also consider
the non-radial component of the solar wind velocity, in the reference frame
of the Sun.
We apply the equation of motion to the motion of dust
grains near commensurability resonances with a planet – mean motion orbital
resonance (MMR; a particle is in resonance with a planet when the ratio of
their mean motions is approximately the ratio of two small integers)
– and possible capture of the grains in the resonances. Up to now, only
nonspherical grains, under action of the electromagnetic radiation of the
central star, were known to exhibit an increase of semimajor axis before
capture into the MMR. This paper shows that the same result can be generated
by the non-radial component of the solar wind even for spherical dust
particles. Spherical dust grains enable the treatment of the problem in an
analytic way (at least partially), which is not the case for the
effect of electromagnetic radiation on nonspherical dust
grains. The situation treated in the paper presents the second known case when
resonant trapping of a cosmic body occurs for diverging orbits. The paper
presents the first case of secular evolution of the eccentricity of a body
captured in the resonance derived in an analytic way for a body
characterized by a diverging orbit
Eccentricity evolution in mean motion resonance and non-radial solar wind
Eccentricity evolution of a dust particle in a mean motion orbital
resonance with a planet in circular orbit is investigated. The action
of solar electromagnetic and corpuscular radiation, including non-radial
components of the solar wind velocity, is taken into account.
Various types of eccentricity evolution depend on the angle between
the radial direction and the direction of the solar wind velocity.
The evolution changes at the analytically derived angles.
Its application to exosolar systems is included