https://hal-insu.archives-ouvertes.fr/insu-03581670Baerenzung, JulienJulienBaerenzungHolschneider, MatthiasMatthiasHolschneiderLesur, VincentVincentLesurIPGP - Institut de Physique du Globe de Paris - UPMC - Université Pierre et Marie Curie - Paris 6 - INSU - CNRS - Institut national des sciences de l'Univers - IPG PARIS - UPD7 - Université Paris Diderot - Paris 7 - UR - Université de La Réunion - CNRS - Centre National de la Recherche ScientifiqueThe flow at the Earth's core-mantle boundary under weak prior constraintsHAL CCSD2016Earth's corecore flowBayesian inversion[SDU] Sciences of the Universe [physics]POTHIER, Nathalie2022-02-20 12:57:112022-02-22 03:36:012022-02-20 12:57:12enJournal articleshttps://hal-insu.archives-ouvertes.fr/insu-03581670/document10.1002/2015JB012464application/pdf1Prior information in ill-posed inverse problem is of critical importance because it is conditioning the posterior solution and its associated variability. The problem of determining the flow evolving at the Earth's core-mantle boundary through magnetic field models derived from satellite or observatory data is no exception to the rule. This study aims to estimate what information can be extracted on the velocity field at the core-mantle boundary, when the frozen flux equation is inverted under very weakly informative, but realistic, prior constraints. Instead of imposing a converging spectrum to the flow, we simply assume that its poloidal and toroidal energy spectra are characterized by power laws. The parameters of the spectra, namely, their magnitudes, and slopes are unknown. The connection between the velocity field, its spectra parameters, and the magnetic field model is established through the Bayesian formulation of the problem. Working in two steps, we determined the time-averaged spectra of the flow within the 2001-2009.5 period, as well as the flow itself and its associated uncertainties in 2005.0. According to the spectra we obtained, we can conclude that the large-scale approximation of the velocity field is not an appropriate assumption within the time window we considered. For the flow itself, we show that although it is dominated by its equatorial symmetric component, it is very unlikely to be perfectly symmetric. We also demonstrate that its geostrophic state is questioned in different locations of the outer core.