A Study of Chaos in the Asteroid Belt

Sidlichovsky, M.; Nesvorný, David

doi:10.1007/978-94-015-9221-5_6

Cited by 13 publications

(14 citation statements)

References 12 publications

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“…However, the influence of the interstellar gas flow on the dynamics of dust particles in the Solar system is usually ignored in the literature. The Poynting–Robertson (PR) effect, the radial solar wind and the gravitational perturbation of a planet (planets) are usually taken into account (Šidlichovský & Nesvorný 1994; Liou & Zook 1997, 1999; Kuchner & Holman 2003).…”

Section: Introductionmentioning

confidence: 99%

Orbital evolution under the action of fast interstellar gas flow

Pástor¹,

Klačka²,

Kómar³

2011

Monthly Notices of the Royal Astronomical Society

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We investigate the orbital evolution of an interplanetary dust particle under the action of an interstellar gas flow. We present the secular time derivatives of the particle's orbital elements, for arbitrary orbit orientation. An important result concerns the secular evolution of the semimajor axis. The secular semimajor axis of the particle on a bound orbit decreases under the action of fast interstellar gas flow. In this paper, we discuss the possible types of evolution of other Keplerian orbital elements. Also, we compare the influences of the Poynting–Robertson effect, the radial solar wind and the interstellar gas flow on the dynamics of the dust particle in the outer planetary region of the Solar system and beyond, up to 100 au. We study the evolution of a putative dust ring in the zone of the Edgeworth–Kuiper belt. The non‐radial solar wind and the gravitational effect of the major planets might have an important role in this zone. We take into account both these effects. The low‐inclination orbits of micrometre‐sized dust particles in the belt are not stable, because of the fast increase of eccentricity caused by the long‐term monodirectional interstellar gas flow and subsequent planetary perturbations – the increase of eccentricity leads to the planet‐crossing orbits of the particles. Gravitational and non‐gravitational effects are treated in a way that fully respects physics. As a consequence, some of the published results have turned out to be incorrect. Moreover, in this paper we treat the problem in a more general way than it has been presented up to now. The influence of the fast interstellar neutral gas flow should not be ignored in the modelling of the evolution of dust particles beyond planets.

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Section: Introductionmentioning

confidence: 99%

Orbital evolution under the action of fast interstellar gas flow

Pástor¹,

Klačka²,

Kómar³

2011

Monthly Notices of the Royal Astronomical Society

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“…The authors considered the motion of spherical interplanetary dust grains near mean-motion orbital resonances with the Earth. Many papers have considered this situation, e.g., Weidenschilling & Jackson (1993), Beaugé & Ferraz-Mello (1994), Marzari & Vanzani (1994), Šidlichovský & Nesvorný (1994), , , Liou & Zook (1997). One of the results of these works was that dust rings around planetary orbits should exist.…”

Section: Introductionmentioning

confidence: 99%

Nonspherical dust grains in mean-motion orbital resonances

Kocifaj

Klačka

2008

A&A

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The effect of stellar electromagnetic radiation on the motion of arbitrarily shaped dust particles in mean-motion orbital resonances with planets is investigated. Giving a resonance and a value of parameter β (the ratio between radiation pressure force and gravitational force of the central star), nonradial components of radiation pressure force are calculated when a given trajectory is prescribed. The found values of the nonradial components are in a good agreement with published detailed numerical simulations for a given nonspherical particle. Therefore nonspherical grains are present in mean-motion resonances with planets. Similarly, the difference between the motion of a real particle and the motion influenced by the Poynting-Robertson effect may be important.

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“…The ring was observed by satellites IRAS (Brownlee 1994;Dermott et al 1994) and COBE (Reach et al 1995). The orbital evolution of interplanetary dust particles near zones of mean motion resonances was investigated in many papers (Weidenschilling & Jackson 1993;Beaugé & Ferraz-Mello 1994;Šidlichovský & Nesvorný 1994;Liou et al 1995;Liou & Zook 1999;Kuchner & Holman 2003;Klačka & Pástor 2004). Liou & Zook (1997) derived the relation between the secular time derivative of eccentricity and the secular time derivative of the inclination of dust particles in mean motion resonance with a planet in a circular restricted three-body problem with the P-R effect and the radial solar wind (the authors incorrectly accounted for the radial solar wind).…”

Section: Introductionmentioning

confidence: 99%

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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A Study of Chaos in the Asteroid Belt

Cited by 13 publications

References 12 publications

Orbital evolution under the action of fast interstellar gas flow

Orbital evolution under the action of fast interstellar gas flow

Nonspherical dust grains in mean-motion orbital resonances

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

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