An iterative method for obtaining a nonlinear solution for the temperature distribution of a rotating spherical body revolving in an eccentric orbit

Sekiya, Minoru; Shimoda, Akihito

doi:10.1016/j.pss.2014.04.006

Cited by 2 publications

(1 citation statement)

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“…These include (i) an inhomogeneity of the thermal parameters (e.g., Vokrouhlický and Brož, 1999), (ii) a coupling of the diurnal and seasonal components of the Yarkovsky effect (e.g., Vokrouhlický, 1999;Shimoda, 2013, 2014), (iii) effects of a non-spherical shape for simple (e.g., Vokrouhlický, 1998b) or general geometries (including non-convex shapes and the role of small-scale surface features; Sec. 2.2), (iv) a non-linearity of the surface boundary condition of the thermal model (e.g., Shimoda, 2013, 2014), (v) the role of very high orbital eccentricity (e.g., Greenberg, 2001, 2002;Sekiya and Shimoda, 2014); (vi) a non-principal axis rotation state (e.g., Vokrouhlický et al, 2005a), or (vii) the Yarkovsky effect for binary asteroids (e.g., Vokrouhlický et al, 2005b).…”

Section: Classical Modelsmentioning

confidence: 99%

The Yarkovsky and YORP Effects

Vokrouhlicky,

Bottke,

Chesley

et al. 2015

Preprint

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The Yarkovsky effect describes a small but significant force that affects the orbital motion of meteoroids and asteroids smaller than 30 − 40 kilometers in diameter. It is caused by sunlight; when these bodies heat up in the Sun, they eventually re-radiate the energy away in the thermal waveband, which in turn creates a tiny thrust. This recoil acceleration is much weaker than solar and planetary gravitational forces, but it can produce measurable orbital changes over decades and substantial orbital effects over millions to billions of years. The same physical phenomenon also creates a thermal torque that, complemented by a torque produced by scattered sunlight, can modify the rotation rates and obliquities of small bodies as well. This rotational variant has been coined the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. During the past decade or so, the Yarkovsky and YORP effects have been used to explore and potentially resolve a number of unsolved mysteries in planetary science dealing with small bodies. Here we review the main results to date, and preview the goals for future work.

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Section: Classical Modelsmentioning

confidence: 99%

The Yarkovsky and YORP Effects

Vokrouhlicky,

Bottke,

Chesley

et al. 2015

Preprint

View full text Add to dashboard Cite

show abstract

The Yarkovsky and YORP Effects

Vokrouhlický¹,

Bottke²,

Chesley³

et al. 2015

Asteroids IV

215

279

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The Yarkovsky effect describes a small but significant force that affects the orbital motion of meteoroids and asteroids smaller than $30-40$ kilometers in diameter. It is caused by sunlight; when these bodies heat up in the Sun, they eventually re-radiate the energy away in the thermal waveband, which in turn creates a tiny thrust. This recoil acceleration is much weaker than solar and planetary gravitational forces, but it can produce measurable orbital changes over decades and substantial orbital effects over millions to billions of years. The same physical phenomenon also creates a thermal torque that, complemented by a torque produced by scattered sunlight, can modify the rotation rates and obliquities of small bodies as well. This rotational variant has been coined the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. During the past decade or so, the Yarkovsky and YORP effects have been used to explore and potentially resolve a number of unsolved mysteries in planetary science dealing with small bodies. Here we review the main results to date, and preview the goals for future work.Comment: Chapter to appear in the Space Science Series Book: Asteroids I

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An iterative method for obtaining a nonlinear solution for the temperature distribution of a rotating spherical body revolving in an eccentric orbit

Cited by 2 publications

References 10 publications

The Yarkovsky and YORP Effects

The Yarkovsky and YORP Effects

The Yarkovsky and YORP Effects

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