An analytical model for YORP and Yarkovsky effects with a physical thermal lag

Mysen, E.

doi:10.1051/0004-6361:20079089

Cited by 11 publications

(19 citation statements)

References 23 publications

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“…To simplify the analytical results we approximate f by using its second order expansion (following [Mysen 2008]):…”

Section: The Yorp Torquementioning

confidence: 99%

“…With numerical models by [Capek & Vokrouhlicky 2004] and [Vokrouhlicky & Capek 2002]. An analytical description of the effect is given, for example, in , in [Scheeres & Mirrahimi 2008] and more recently in [Mysen 2008]. As the YORP torque is a small torque, it can be treated as a perturbation to the unperturbed rotational motion, and the important effects are then secular ones over long time spans.…”

Section: Introductionmentioning

confidence: 99%

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Averaged rotational dynamics of an asteroid in tumbling rotation under the YORP torque

Cicalò

Scheeres²

2010

Celest Mech Dyn Astr

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The secular effect of YORP torque on the rotational dynamics of an asteroid in non-principal axis rotation is studied. The general rotational equations of motion are derived and approximated with an illumination function expanded up to second order. The resulting equations of motion can be averaged over the fast rotation angles to yield secular equations for the angular momentum, dynamic inertia and obliquity. We study the properties of these secular equations and compare results to previous research. Finally, an application to several real asteroid shapes is made, in particular we study the predicted rotational dynamics of the asteroid Toutatis, which is known to be in a non-principal axis state.

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“…To simplify the analytical results we approximate f by using its second order expansion (following [Mysen 2008]):…”

Section: The Yorp Torquementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Averaged rotational dynamics of an asteroid in tumbling rotation under the YORP torque

Cicalò

Scheeres²

2010

Celest Mech Dyn Astr

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“…All known recipes for computing the YORP torques can be roughly divided in two main groups: most of them use a discrete mesh, summing the contributions from each triangular face (Vokrouhlický &Čapek 2002;Čapek & Vokrouhlický 2004;Scheeres 2007;Statler 2009), whereas others use a continuous shape model described in terms of spherical harmonics (Breiter & Michalska 2008;Mysen 2008;Nesvorný & Vokrouhlický 2008). The latter group cannot be applied to Itokawa, because its irregular shape, not being starlike, cannot be expressed in terms of spherical harmonics.…”

Section: Computational Modelmentioning

confidence: 99%

“…Čapek & Vokrouhlický (2004), Scheeres (2007), , Mysen (2008), Nesvorný & Vokrouhlický (2008), and Breiter & Michalska (2008) use various approximations to account for the nonzero conductivity. Their thermal models use a "plane parallel" approximation reducing the problem to a 1D heat diffusion model.…”

Section: Computational Modelmentioning

confidence: 99%

The YORP effect on 25 143 Itokawa

Breiter

Bartczak

Czekaj

et al. 2009

A&A

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Context. The asteroid 25143 Itokawa is one of the candidates for the detection of the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect in the rotation period. Previous studies were carried out up to the 196 608 facets triangulation model and were not able to provide a good theoretical estimate of this effect, raising questions about the influence of the mesh resolution and the centre of mass location on the evolution the rotation period. Aims. The YORP effect on Itokawa is computed for different topography models up to the highest resolution Gaskell mesh of 3 145 728 triangular faces in an attempt to find the best possible YORP estimate. Other, lower resolution models are also studied and the question of the dependence of the rotation period drift on the density distribution inhomogeneities is reexamined. A comparison is made with 433 Eros models possessing a similar resolution. Methods. The Rubincam approximation (zero conductivity) is assumed in the numerical simulation of the YORP effect in rotation period. The mean thermal radiation torques are summed over triangular facets assuming Keplerian heliocentric motion and uniform rotation around a body-fixed axis.Results. There is no evidence of YORP convergence in Gaskell model family. Differently simplified meshes may converge quickly to their parent models, but this does not prove the quality of YORP computed from the latter. We confirm the high sensitivity of the YORP effect to the fine details of the surface for 25 143 Itokawa and 433 Eros. The sensitivity of the Itokawa YORP to the centre of mass shift is weaker than in earlier works, but instead the results prove to be sensitive to the spin axis orientation in the body frame. Conclusions. Either the sensitivity of the YORP effect is a physical phenomenon and all present predictions are questionable, or the present thermal models are too simplified.

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“…Convex bodies admit the simplest form of the illumination factor ν, a function of unit outward normal to the surface and the solar direction , namely because no shadows are cast by one surface element on another. Mysen (2008) and Cicaló & Scheeres (2010) approximate ν using either truncated Fourier series of the Sun’s zenith distance z s or its conversion to the polynomial of . The former is not well adapted to further analytical treatment, whereas the latter requires the replacement of all coefficients when changing the maximum degree of the polynomial.…”

Section: Yorp Torquementioning

confidence: 99%

Yarkovsky-O’Keefe-Radzievskii-Paddack effect on tumbling objects

Breiter¹,

Rożek²,

Vokrouhlický³

2011

Monthly Notices of the Royal Astronomical Society

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A semi-analytical model of the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect on an asteroid spin in a non-principal axis rotation state is developed. The model describes the spin-state evolution in Deprit-Elipe variables, first-order averaged with respect to rotation and Keplerian orbital motion. Assuming zero conductivity, the YORP torque is represented by spherical harmonic series with vectorial coefficients, allowing us to use any degree and order of approximation. Within the quadrupole approximation of the illumination function we find the same first integrals involving rotational momentum, obliquity and dynamical inertia that were obtained by Cicaló & Scheeres. The integrals do not exist when higher degree terms of the illumination function are included, and then the asymptotic states known from Vokrouhlický et al. appear. This resolves an apparent contradiction between earlier results. Averaged equations of motion admit stable and unstable limit cycle solutions that were not previously detected. Non-averaged numerical integration by the Taylor series method for an exemplary shape of 3103 Eger is in good agreement with the semi-analytical theory.

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An analytical model for YORP and Yarkovsky effects with a physical thermal lag

Cited by 11 publications

References 23 publications

Averaged rotational dynamics of an asteroid in tumbling rotation under the YORP torque

Averaged rotational dynamics of an asteroid in tumbling rotation under the YORP torque

The YORP effect on 25 143 Itokawa

Yarkovsky-O’Keefe-Radzievskii-Paddack effect on tumbling objects

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