The Yarkovsky and YORP Effects

Vokrouhlicky, D.; Bottke, W. F.; Chesley, S. R.; Scheeres, D. J.; Statler, T. S.

doi:10.48550/arxiv.1502.01249

Cited by 3 publications

(3 citation statements)

References 106 publications

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“…The spin-up of submicron grains by solar radiation is analogous to the YORP (Yarkovsky-O'Keefe-Radzievskii-Paddack) effect (see Vokrouhlicky et al (2015) for a review), but where the irregularities are on scales comparable to the wavelength. Dust grains have far higher critical angular velocities for disruption than rubble piles because the former are held together by chemical bonds rather than gravity.…”

Section: Torquesmentioning

confidence: 99%

Radiation Pressure on Fluffy Submicron-Sized Grains

Silsbee

Draine

2016

ApJ

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We investigate the claim that the ratio β of radiation pressure force to gravitational force on a dust grain in our solar system can substantially exceed unity for some grain sizes, provided that grain porosity is high enough. For model grains consisting of random aggregates of silicate spherules, we find that the maximum value of β is almost independent of grain porosity, but for small (< 0.3µm) grains, β actually decreases with increasing porosity. We also investigate the effect of metallic iron and amorphous carbon inclusions in the dust grains and find that while these inclusions do increase the radiation pressure cross-section, β remains below unity for grains with 3 pg of silicate material. These results affect the interpretation of the grain trajectories estimated from the Stardust mission, which were modeled assuming β values exceeding one. We find that radiation pressure effects are not large enough for particles Orion and Hylabrook captured by Stardust to be of interstellar origin given their reported impact velocities. We also consider the effects of solar radiation on transverse velocities and grain spin, and show that radiation pressure introduces both transverse velocities and equatorial spin velocities of several hundred meters per second for incoming interstellar grains at 2 AU. These transverse velocities are not important for modeling trajectories, but such spin rates may result in centrifugal disruption of aggregates.

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Section: Torquesmentioning

confidence: 99%

Radiation Pressure on Fluffy Submicron-Sized Grains

Silsbee

Draine

2016

ApJ

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“…The Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect alters the rotation rate of asteroids and the orientations of their rotation axes (Rubincam 2000;Bottke et al 2006;Vokrouhlický et al 2015). The vector of the YORP torque has 3 components.…”

Section: Introductionmentioning

confidence: 99%

Physical models for the normal YORP and diurnal Yarkovsky effects

Golubov

Kravets

Krugly³

et al. 2016

Mon. Not. R. Astron. Soc.

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We propose an analytic model for the normal YORP and diurnal Yarkovsky effects experienced by a convex asteroid. Both the YORP torque and the Yarkovsky force are expressed as integrals of a universal function over the surface of an asteroid. Although in general this function can only be calculated numerically from the solution of the heat conductivity equation, approximate solutions can be obtained in quadratures for important limiting cases. We consider 3 such simplified models: Rubincam's approximation (zero heat conductivity), low thermal inertia limit (including the next order correction and thus valid for small heat conductivity), and high thermal inertia limit (valid for large heat conductivity). All three simplified models are compared with the exact solution.

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“…The Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect is the torque experienced by an asteroid due to its asymmetric emission of incident light pressure radiation by its surface (Rubincam, 2000;Bottke et al, 2006;Vokrouhlický et al, 2015). It is useful to divide the YORP torque into two components.…”

Section: Introductionmentioning

confidence: 99%

Obliquity dependence of the tangential YORP

Ševeček

Golubov

Scheeres

et al. 2016

A&A

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Context. The tangential Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect is a thermophysical effect that can alter the rotation rate of asteroids and is distinct from the so-called normal YORP effect, but to date has only been studied for asteroids with zero obliquity. Aims. We aim to study the tangential YORP force produced by spherical boulders on the surface of an asteroid with an arbitrary obliquity. Methods. A finite element method is used to simulate heat conductivity inside a boulder, to find the recoil force experienced by it. Then an ellipsoidal asteroid uniformly covered by these types of boulders is considered and the torque is numerically integrated over its surface. Results. Tangential YORP is found to operate on non-zero obliquities and decreases by a factor of two for increasing obliquity.

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The Yarkovsky and YORP Effects

Cited by 3 publications

References 106 publications

Radiation Pressure on Fluffy Submicron-Sized Grains

Radiation Pressure on Fluffy Submicron-Sized Grains

Physical models for the normal YORP and diurnal Yarkovsky effects

Obliquity dependence of the tangential YORP

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