The non-radial component of the solar wind and motion of dust near mean motion resonances with planets

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

doi:10.1051/0004-6361:20078752

Cited by 12 publications

(14 citation statements)

References 25 publications

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“…If the initial eccentricity equals 0, then the derivation of Eq. (7) does not allow any conclusions since the partial derivative of the Tisserand parameter with respect to eccentricity is 0 (see Klačka et al 2008).…”

Section: Evolution Of Eccentricity In a Mean Motion Resonancementioning

confidence: 99%

“…The orbital evolution in mean motion resonance in the planar elliptical restricted three-body problem with the P-R effect is discussed in Pástor et al (2007). The evolution of eccentricity of the particle under the action of the P-R effect and the non-radial solar wind in mean motion resonances with a planet in a circular orbit is investigated in Klačka et al (2008). Measurement of the non-radial component of the solar wind velocity was performed by Helios 2 during its first solar mission in 1976 (Bruno et al 2003).…”

Section: Introductionmentioning

confidence: 99%

“…We are motivated mainly by the results of Klačka et al (2008). We want to obtain detailed predictions of orbital evolution in the orbital resonances when the P-R effect and the nonradial solar wind are considered.…”

Section: Introductionmentioning

confidence: 99%

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

Pástor¹,

Klačka²,

Petržala³

et al. 2009

A&A

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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.

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Section: Evolution Of Eccentricity In a Mean Motion Resonancementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Pástor¹,

Klačka²,

Petržala³

et al. 2009

A&A

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“…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%

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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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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The non-radial component of the solar wind and motion of dust near mean motion resonances with planets

Cited by 12 publications

References 25 publications

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

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

Solar wind and the motion of dust grains

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

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