Eccentricity evolution in mean motion resonance and non-radial solar wind

Pástor, P.; Klačka, J.; Petržala, Jaromír; Kómar, Ladislav

doi:10.1051/0004-6361/200811286

Cited by 7 publications

(9 citation statements)

References 32 publications

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“…The acceleration caused by the solar wind was used in Klačka et al (2008) and Pástor et al (2009a) without one term of the second order in v / u , as follows from the covariant formulation and equations () and (). However, as we see, the new term does not have any influence on the secular considerations in Klačka et al (2008) and Pástor et al (2009a).…”

Section: Secular Evolution Of a Particle’s Orbital Elements Under Tmentioning

confidence: 99%

“…The non‐radial component of the solar wind velocity vector has also been considered in the equation of motion to the first order of v / u (Klačka 1994). Klačka et al (2008) and Pástor et al (2009a) used the acceleration caused by the non‐radial solar wind to the second order in v / u . The acceleration in Klačka et al (2008) and Pástor et al (2009a) was used without one term of the second order in v / u , as follows from the covariant formulation presented in this paper.…”

Section: Introductionmentioning

confidence: 99%

“…Klačka et al (2008) and Pástor et al (2009a) used the acceleration caused by the non‐radial solar wind to the second order in v / u . The acceleration in Klačka et al (2008) and Pástor et al (2009a) was used without one term of the second order in v / u , as follows from the covariant formulation presented in this paper. We explicitly present the complete acceleration caused by the non‐radial solar wind to the second order in v / u .…”

Section: Introductionmentioning

confidence: 99%

“…Klačka et al (2008) used the acceleration from the P–R effect and the non‐radial solar wind in order to obtain the properties of the orbital evolutions of dust particles near to (or captured in) a mean‐motion resonance with a planet. Pástor et al (2009a) analysed in detail all possibilities of the secular evolutions of eccentricity in a mean‐motion resonance with a planet under the action of the P–R effect and the non‐radial solar wind.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Solar wind and the motion of dust grains

Klačka

Petržala

Pástor

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In this paper, we investigate the action of solar wind on an arbitrarily shaped interplanetary dust particle. The final relativistically covariant equation of motion of the particle also contains the change of the particle’s mass. The non‐radial solar wind velocity vector is also included. The covariant equation of motion reduces to the Poynting–Robertson effect in the limiting case when a spherical particle is treated, when the speed of the incident solar wind corpuscles tends to the speed of light and when the corpuscles spread radially from the Sun. The results of quantum mechanics have to be incorporated into the physical considerations, in order to obtain the limiting case. If the solar wind affects the motion of a spherical interplanetary dust particle, then . Here, p′in and p′out are the incoming and outgoing radiation momenta (per unit time), respectively, measured in the proper frame of reference of the particle, and and are the solar wind pressure and the total scattering cross‐sections, respectively. An analytical solution of the derived equation of motion yields a qualitative behaviour consistent with numerical calculations. This also holds if we consider a decrease of the particle’s mass. Using numerical integration of the derived equation of motion, we confirm our analytical result that the non‐radial solar wind (with a constant value of angle between the radial direction and the direction of the solar wind velocity) causes outspiralling of the dust particle from the Sun for large values of the particle’s semimajor axis. The non‐radial solar wind also increases the time the particle spirals towards the Sun. If we consider the periodical variability of the solar wind with the solar cycle, then there are resonances between the particle’s orbital period and the period of the solar cycle.

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Section: Secular Evolution Of a Particle’s Orbital Elements Under Tmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Solar wind and the motion of dust grains

Klačka

Petržala

Pástor

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…However, the role of it on motion close to mean motion-resonances is still unclear. Previous studies [Sicardy et al, 1993, Beauge and Ferraz-Mello, 1994, Beauge, 1994, Liou and Zook, 1997, Jancart et al, 2003, Klačka and Kocifaj, 2008, Pástor et al, 2009, Kocifaj and Kundracik, 2012, Pástor, 2014, Lhotka and Celletti, 2015, Pástor, 2016 investigated the dynamical problem under the assumption that dust is uncharged. This assumption is only valid in the case where the dust grain is heavy enough and where the magnitude of the Lorentz force is much smaller compared to the magnitudes of the other ones.…”

Section: Introductionmentioning

confidence: 99%

Charged dust close to outer mean-motion resonances in the heliosphere

Lhotka

Galeş

2019

Celest Mech Dyn Astr

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We investigate the dynamics of charged dust close to outer meanmotion resonances with planet Jupiter. The importance of the interplanetary magnetic field on the orbital evolution of dust is clearly demonstrated. New dynamical phenomena are found that do not exist in the classical problem of uncharged dust. We find changes in the orientation of the orbital planes of dust particles, an increased amount of chaotic orbital motions, sudden 'jumps' in the resonant argument, and a decrease in time of temporary capture due to the Lorentz force. Variations in the orbital planes of dust grain orbits are found to be related to the angle between the orbital angular momentum and magnetic axes of the heliospheric field and the rotation rate of the Sun. These variations are bound using a simplified model derived from the full dynamical problem using first order averaging theory. It is found that the interplanetary magnetic field does not affect the capture process, that is still dominated by the other non-gravitational forces. Our study is based on a dynamical model in the framework of the inclined circular restricted three-body problem. Additional forces include solar radiation pressure, solar wind drag, the Poynting-Robertson effect, and the influence of a Parker spiral type interplanetary magnetic field model. The analytical estimates are derived on the basis of Gauss' form of planetary equations of motion. Numerical results are obtained by simulations of dust grain orbits together with the system of variational equations. Chaotic regions in phase space are revealed by means of Fast Lyapunov Chaos Indicators.

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On the stability of dust orbits in mean-motion resonances perturbed by from an interstellar wind

Pástor¹

2014

Celest Mech Dyn Astr

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Circumstellar dust particles can be captured in a mean motion resonance with a planet and simultaneously be affected by non-gravitational effects. It is possible to describe the secular variations of a particle orbit in the mean motion resonance analytically using averaged resonant equations. We derive the averaged resonant equations from the equations of motion in near-canonical form. The secular variations of the particle orbit depending on the orientation of the orbit in space are taken into account. The averaged resonant equations can be derived/confirmed also from Lagrange's planetary equations. We apply the derived theory to the case when the non-gravitational effects are the Poynting-Robertson effect, the radial stellar wind, and an interstellar wind. The analytical and numerical results obtained are in excellent agreement. We found that the types of orbits correspond to libration centers of the conservative problem. The averaged resonant equations can lead to a system of equations which hold for stationary points in a subset of resonant variables. Using this system we show analytically that for the considered non-gravitational effects, all stationary points should correspond to orbits which are stationary in interplanetary space after an averaging over a synodic period. In an exact resonance, the stationary orbits are stable. The stability is achieved by a periodic repetition of the evolution during the synodic period. Numerical solutions of this system show that there are no stationary orbits for either the exact or non-exact resonances.

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Eccentricity evolution in mean motion resonance and non-radial solar wind

Cited by 7 publications

References 32 publications

Solar wind and the motion of dust grains

Solar wind and the motion of dust grains

Charged dust close to outer mean-motion resonances in the heliosphere

On the stability of dust orbits in mean-motion resonances perturbed by from an interstellar wind

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