The Poynting–Robertson effect: A critical perspective

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

doi:10.1016/j.icarus.2012.06.044

Cited by 33 publications

(39 citation statements)

References 24 publications

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“…Also, Burns et al (2014) explain that the primed quantities used in their equation are equivalent to the unprimed values in equation (5) to low order in v/c; this difference in quantities has previously been identified (Klačka et al 2014). …”

Section: Acceleration Due To Absorbed Radiationmentioning

confidence: 89%

The orbital evolution of asteroids, pebbles and planets from giant branch stellar radiation and winds

Veras¹,

Eggl²,

Gänsicke³

2015

Monthly Notices of the Royal Astronomical Society

104

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The discovery of over 50 planets around evolved stars and more than 35 debris discs orbiting white dwarfs highlight the increasing need to understand small body evolution around both early and asymptotic giant branch (GB) stars. Pebbles and asteroids are susceptible to strong accelerations from the intense luminosity and winds of GB stars. Here, we establish equations that can model time-varying GB stellar radiation, wind drag and mass loss. We derive the complete three-dimensional equations of motion in orbital elements due to (1) the Epstein and Stokes regimes of stellar wind drag, (2) Poynting-Robertson drag, and (3) the Yarkovsky drift with seasonal and diurnal components. We prove through averaging that the potential secular eccentricity and inclination excitation due to Yarkovsky drift can exceed that from PoyntingRobertson drag and radiation pressure by at least three orders of magnitude, possibly flinging asteroids which survive YORP spin-up into a widely dispersed cloud around the resulting white dwarf. The GB Yarkovsky effect alone may change an asteroid's orbital eccentricity by ten per cent in just one Myr. Damping perturbations from stellar wind drag can be just as extreme, but are strongly dependent on the highly uncertain local gas density and mean free path length. We conclude that GB radiative and wind effects must be considered when modelling the post-main-sequence evolution of bodies smaller than about 1000 km.

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Section: Acceleration Due To Absorbed Radiationmentioning

confidence: 89%

The orbital evolution of asteroids, pebbles and planets from giant branch stellar radiation and winds

Veras¹,

Eggl²,

Gänsicke³

2015

Monthly Notices of the Royal Astronomical Society

104

View full text Add to dashboard Cite

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“…[21], and references therein). Recently, a debate regarding the physical foundations of PR effect between Klačka et al and Burns et al has appeared in the literature [38][39][40].…”

Section: Discussion and Interpretation Of The Obtained Resultsmentioning

confidence: 99%

Poynting-Robertson effect as a dissipative system in general relativity

Falco

Battista

2020

Phys. Rev. D

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We determine for the first time in the literature the analytic form of the Rayleigh potential of the general relativistic Poynting-Robertson effect. The employed procedure is based on the use of an integrating factor and a new integration strategy where the test particle's dissipated energy represents the fundamental variable. The obtained results and their implications are discussed. Finally, concluding remarks and future projects are drawn. * vittorio.defalco@physics.cz †

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“…The acceleration of moving spherical dust particles caused by the electromagnetic radiation is the PR effect (Poynting 1904;Robertson 1937;Klačka 1992Klačka , 2004Klačka et al 2014). The acceleration is…”

Section: Electromagnetic Radiationmentioning

confidence: 99%

Properties of interstellar wind leading to shape morphology of the dust surrounding HD 61005

Pástor¹

2017

A&A

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Aims. A structure formed by dust particles ejected from the debris ring around HD 61005 is observed in the scattered light. The main aim here is to constrain interstellar wind parameters that lead to shape morphology in the vicinity of HD 61005 using currently available observational data for the debris ring. Methods. Equation of motion of 2 × 10 5 dust particles ejected from the debris ring under the action of the electromagnetic radiation, stellar wind, and interstellar wind is solved. A two-dimensional (2D) grid is placed in a given direction for accumulation of the light scattered on the dust particles in order to determine the shape morphology. The interaction of the interstellar wind and the stellar wind is considered. Results. Groups of unknown properties of the interstellar wind that create the observed morphology are determined. A relation between number densities of gas components in the interstellar wind and its relative velocity is found. Variations of the shape morphology caused by the interaction with the interstellar clouds of various temperatures are studied. When the interstellar wind velocity is tilted from debris ring axis a simple relation between the properties of the interstellar wind and an angle between the line of sight and the interstellar wind velocity exists. Dust particles that are most significantly influenced by stellar radiation move on the boundary of observed structure. Conclusions. Observed structure at HD 61005 can be explained as a result of dust particles moving under the action of the interstellar wind. Required number densities or velocities of the interstellar wind are much higher than that of the interstellar wind entering the Solar system.

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The Poynting–Robertson effect: A critical perspective

Cited by 33 publications

References 24 publications

The orbital evolution of asteroids, pebbles and planets from giant branch stellar radiation and winds

The orbital evolution of asteroids, pebbles and planets from giant branch stellar radiation and winds

Poynting-Robertson effect as a dissipative system in general relativity

Properties of interstellar wind leading to shape morphology of the dust surrounding HD 61005

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