Dynamical Effects of Radiation in the Solar System

Robertson, H. P.; Russell, Henry Norris

doi:10.1093/mnras/97.6.423

Cited by 431 publications

(301 citation statements)

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“…The case e > 1 describes the case when the particle is ejected from the Solar System. (40), we obtain Poynting-Robertson effect (Robertson 1937, Klačka 1992a:…”

Section: Klačka 1992b)mentioning

confidence: 93%

“…The second case, closely connected with the relativistic equation of motion for a free particle under the action of electromagnetic radiation, was presented by Einstein (1905), who calculated the change of energy and light pressure at arbitrary angle of incidence on a plane mirror. Robertson (1937) subsequently derived a correct equation of motion for a perfectly absorbing spherical particle. This result has been applied to astronomical problems for several decades and is known as the Poynting-Robertson (P-R) effect.…”

Section: Introductionmentioning

confidence: 99%

“…Some others will be mentioned within the context of the discussed problems. Since some confusion exists in presenting derivations and results in the most cited papers (Robertson 1937;Wyatt and Whipple 1950;Burns et al 1979;Mignard 1992), we present detailed derivation of the secular changes of orbital elements for heliocentric orbits and the P-R effect.…”

Section: Introductionmentioning

confidence: 99%

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Electromagnetic Radiation and Motion of a Particle

Klačka

2004

Celestial Mechanics and Dynamical Astronomy

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Abstract. We consider the motion of uncharged dust grains of arbitrary shape including the effects of electromagnetic radiation and thermal emission. The resulting relativistically covariant equation of motion is expressed in terms of standard optical parameters.Explicit expressions for secular changes of osculating orbital elements are derived in detail for the special case of the Poynting-Robertson effect. Two subcases are considered: (i) central acceleration due to gravity and the radial component of radiation pressure independent of the particle velocity, (ii) central acceleration given by gravity and the radiation force as the disturbing force. The latter case yields results which may be compared with secular orbital evolution in terms of orbital elements for an arbitrarily shaped dust particle. The effects of solar wind are also presented.

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“…The case e > 1 describes the case when the particle is ejected from the Solar System. (40), we obtain Poynting-Robertson effect (Robertson 1937, Klačka 1992a:…”

Section: Klačka 1992b)mentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Electromagnetic Radiation and Motion of a Particle

Klačka

2004

Celestial Mechanics and Dynamical Astronomy

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“…The improved derivation take into account arbitrary optical properties of particle with material distributed in a spherically symmetric way. The improved derivation leads to the same result for the case considered in Robertson (1937). The relativistic derivation of the PR effect can be generalized also for the solar wind.…”

Section: Introductionmentioning

confidence: 58%

Positions of equilibrium points for dust particles in the circular restricted three-body problem with radiation

Pástor¹

2014

Monthly Notices of the Royal Astronomical Society

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For a body with negligible mass moving in the gravitational field of a star and one planet in a circular orbit (the circular restricted three-body problem) five equilibrium points exist and are known as the Lagrangian points. The positions of the Lagrangian points are not valid for dust particles because in the derivation of the Lagrangian points is assumed that no other forces beside the gravitation act on the body with negligible mass. Here we determined positions of the equilibrium points for the dust particles in the circular restricted three-body problem with radiation. The equilibrium points are located on curves connecting the Lagrangian points in the circular restricted threebody problem. The equilibrium points for Jupiter are distributed in large interval of heliocentric distances due to its large mass. The equilibrium points for the Earth explain a cloud of dust particles trailing the Earth observed with the Spitzer Space Telescope. The dust particles moving in the equilibrium points are distributed in interplanetary space according to their properties.

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“…Again, we would expect to see a change as the spacecraft spins down. A final possibility is the Poynting Robertson effect [Robertson, 1937]. This effect, which is viewed in celestial mechanics as an aberration, is due to the conservation of momentum of photons reradiated from the satellite both along and opposite the motion.…”

Section: Analysis Of the Datamentioning

confidence: 99%

Applications of Geodesy to Geodynamics an International Symposium

Mueller

1977

Bull. Geodesique

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Dynamical Effects of Radiation in the Solar System

Cited by 431 publications

References 0 publications

Electromagnetic Radiation and Motion of a Particle

Electromagnetic Radiation and Motion of a Particle

Positions of equilibrium points for dust particles in the circular restricted three-body problem with radiation

Applications of Geodesy to Geodynamics an International Symposium

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