000004685 001__ 4685
000004685 005__ 20200128201346.0
000004685 037__ $$aCTALK-2020-0073
000004685 100__ $$aRivoldini, Attilio
000004685 245__ $$aNon-hydrostatic effects on Mars’ nutation
000004685 260__ $$c2019
000004685 269__ $$c2019-09-17
000004685 520__ $$aMars’ tidally forced nutation can be resonantly ampli- fied owing to a rotational normal mode called the Free Core Nutation (FCN) which exists because the mantle and fluid part of the core can have a relative rotational motion [1]. The period of the FCN and the amplitude of the nutation depend on the moments of inertia of the mantle and core, as well as on the deformation of the planet due to rotation rate variations and tidal forcing. One of the goals of the RISE experiment on InSight [2] and of the future LaRa experiment on ExoMars 2020 is to infer the core radius of Mars by measuring nuta- tion. Precise core radius determination from the FCN period requires knowledge of the core shape. Here we study how non-hydrostatic core shape models affect the FCN and discuss to what extent the shape of the core could be inferred if its radius were known.
000004685 594__ $$aNO
000004685 700__ $$aBeuthe, Mikael
000004685 700__ $$aVan Hoolst, Tim
000004685 700__ $$aWieczorek, Mark
000004685 700__ $$aBaland, Rose-Marie
000004685 700__ $$aDehant, Véronique
000004685 700__ $$aFolkner, Bill
000004685 700__ $$aLe Maistre, Sébastien
000004685 700__ $$aPéters, Marie-Julie Peters
000004685 700__ $$aYseboodt , Marie
000004685 773__ $$tEPSC-DPS2019 Geneva
000004685 8560_ $$fattilio.rivoldini@observatoire.be
000004685 8564_ $$s8005258$$uhttps://publi2-as.oma.be/record/4685/files/rivoldini.pdf
000004685 8564_ $$s5200$$uhttps://publi2-as.oma.be/record/4685/files/rivoldini.gif?subformat=icon$$xicon
000004685 8564_ $$s6531$$uhttps://publi2-as.oma.be/record/4685/files/rivoldini.jpg?subformat=icon-180$$xicon-180
000004685 906__ $$aContributed
000004685 980__ $$aCTALKCONT