EGU2020-5324
https://doi.org/10.5194/egusphere-egu2020-5324
EGU General Assembly 2020
© Author(s) 2022. This work is distributed under
the Creative Commons Attribution 4.0 License.

The nutations of a rigid Mars

Rose-Marie Baland, Marie Yseboodt, Sébastien Le Maistre, Attilio Rivoldini, Tim Van Hoolst, and Véronique Dehant
Rose-Marie Baland et al.
  • Royal Observatory of Belgium, Uccle, Belgium (rose-marie.baland@oma.be)

The nutations of Mars are about to be estimated with unprecedented accuracy (a few milliarcseconds) with the radioscience experiments RISE (Rotation and Interior Structure Experiment, Folkner et al. 2018) and LaRa (Lander Radioscience, Dehant et al. 2020) of the InSight and ExoMars 2020 missions, allowing to detect the contributions due to the liquid core and tidal deformations and to constrain the interior of Mars.

To properly identify the non-rigid contribution, an accurate precession and nutation model for a rigidly behaving Mars is needed. We develop such a model, based on the Torque approach, and include the forcings by the Sun, Phobos, Deimos, and the other planets of the Solar System, as well as geodetic precession and nutations. Both semi-analytical developments (for the Solar and planetary torques) and analytical solutions (for Phobos and Deimos torques and the geodetic precession and nutations) are considered.

We identify 43 nutation terms with an amplitude above the chosen truncation criterion of 0.025 milliarcseconds in prograde and/or retrograde nutations. Uncertainties related to modelling choices are negligible in comparison to the uncertainty coming from the observational uncertainty on the current determination of the precession rate of Mars (7608.3+/-pm2.1 mas/yr, Konopliv et al. 2016). Our model predicts a dynamical flattening HD=(C-A)/C=0.00538017+/-0.00000148 and a normalized polar moment of inertia C/MR2=0.36367+/-0.00010 for Mars.

References:
Folkner et al., 2018. doi: 10.1007/s11214-018-0530-5.
Dehant et al., 2020. doi: 10.1016/j.pss.2019.104776.
Konopliv et al., 2016. doi: 10.1016/j.icarus.2016.02.052.

How to cite: Baland, R.-M., Yseboodt, M., Le Maistre, S., Rivoldini, A., Van Hoolst, T., and Dehant, V.: The nutations of a rigid Mars, EGU General Assembly 2020, Online, 4–8 May 2020, EGU2020-5324, https://doi.org/10.5194/egusphere-egu2020-5324, 2020.

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  • CC1: Comment on EGU2020-5324, Joana S. Oliveira, 01 May 2020

    Thank you for posting this! In your table you do not mention the Earth's Moon however, even if much smaller than Venus, it is also much closer to Mars. Is there any reason to not consider its impact on Mars nutation? Thanks!

    • AC1: Reply to CC1, Rose-Marie Baland, 02 May 2020

      Thanks for the question.

      In fact we consider the Earth-Moon barycenter (EBM). We have checked that considering the Earth or the EBM does not significantly change the nutation solution. This is because the mass of the Moon is only about 1% of the Earth mass, and the barycenter is only about 1 % of the Earth-Moon distance.

      • AC2: Reply to AC1, Rose-Marie Baland, 02 May 2020

        (EMB, not EBM)