Specific effects of large asteroids on the orbits of terrestrial planets and the ASETEP database

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Volume 540 (April 2012)

A&A, 540 (2012) A21

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Issue		A&A Volume 540, April 2012


Article Number		A21
Number of page(s)		25
Section		Celestial mechanics and astrometry
DOI		https://doi.org/10.1051/0004-6361/201118564
Published online		19 March 2012

Online material

Appendix A: Effects on the Mars orbital motion

Table A.1

Coefficients of Fourier and Poisson series for the effects of Ceres on e_Mars.

	Fig. A.1 Effects of Ceres on e_Mars for a 100 y time interval from JJ 2009.81; raw signal (in black), fitting curve (in red) and residuals (in green).
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Table A.2

Coefficients of Fourier and Poisson series for the effects of Ceres on i_Mars.

	Fig. A.2 Effects of Ceres on i_Mars for a 100 y time interval from JJ 2009.81; raw signal (in black), fitting curve (in red) and residuals (in green).
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Table A.3

Coefficients of Fourier and Poisson series for the effects of Ceres on Ω_Mars.

	Fig. A.3 Effects of Ceres on Ω_Mars for a 100 y time interval from JJ 2009.81; raw signal (in black), fitting curve (in red) and residuals (in green).
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Table A.4

Coefficients of Fourier and Poisson series for the effects of Ceres on .

	Fig. A.4 Effects of Ceres on for a 100 y time interval from JJ 2009.81; raw signal (in black), fitting curve (in red) and residuals (in green).
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Table A.5

Coefficients of Fourier and Poisson series for the effects of Pallas on a_Mars.

Table A.6

Coefficients of Fourier and Poisson series for the effects of Vesta on a_mars.

Appendix B: individual and combined asteroidal effects

	Fig. B.1 Combined effects of the 43 asteroids on e_Mars. The curve in green represents the difference between two ways of computation: adding individual perturbations, or making a combined integration.
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	Fig. B.2 Zoom of the green curve of Fig. B.1, showing the difference between two ways of computation.
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	Fig. B.3 Combined effects of the 43 asteroids on i_Mars. The curve in green represents the difference between two ways of computation: adding individual perturbations, or making a combined integration.
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	Fig. B.4 Zoom of the green curve of Fig. B.3, showing the difference between two ways of computation.
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	Fig. B.5 Combined effects of the 43 asteroids on Ω_Mars. The curve in green represents the difference between two ways of computation: adding individual perturbations, or making a combined integration.
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	Fig. B.6 Zoom of the green curve of Fig. B.5, showing the difference between two ways of computation.
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	Fig. B.7 Combined effects of the 43 asteroids on . The curve in green represents the difference between two ways of computation: adding individual perturbations, or making a combined integration.
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	Fig. B.8 Zoom of the green curve of Fig. B.7, showing the difference between two ways of computation.
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	Fig. B.9 Combined effects of the 43 asteroids on λ_Mars. The curve in green represents the difference between two ways of computation: adding individual perturbations, or making a combined integration.
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	Fig. B.10 Zoom of the green curve of Fig. B.9, showing the difference between two ways of computation.
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Appendix C: Use of ASTEP for ephemerides study

	Fig. C.1 Uncertainty of the EMB-to-Mars distance due to the lack of accuracy in Pallas’ mass (red curve) and difference in the EMB-to-Mars distance between DE405 and INPOP08 (black curve).
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	Fig. C.2 Uncertainty of the EMB-to-Mars distance due to the lack of accuracy in Vesta’s mass (red curve) and difference in the EMB-to-Mars distance between DE405 and INPOP08 (black curve).
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© ESO, 2012

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