01721nas a2200157   4500000000100000000000100001008004100002100002300043700001700066700002300083245012100106856004300227300001400270490000800284520127100292       2022                            d1 aAntonios Nathanail1 aPrasun Dhang1 aChristian M. Fromm00aMagnetic field structure in the vicinity of a supermassive black hole in low-luminosity galaxies: the case of Sgr A*  uhttps://doi.org/10.1093/mnras/stac1276  a5204-52100 v5133 aObservations of SgrA∗ have provided a lot of insight on low-luminosity accretion, with a handful of bright flares accompanied with orbital motion close to the horizon. It has been proposed that gas supply comes from stellar winds in the neighborhood of the supermassive black hole. We here argue that the flow at the vicinity of the black hole has a low magnetization and a structure of alternating polarity, totally dictated by the well-studied and long-ago proposed MRI turbulent process. This can be the case, provided that in larger distances from the black hole magnetic diffusivity is dominant, and thus, the magnetic field will never reach equipartition values. For SgrA∗⁠, we show the immediate consequences of this specific magnetic field geometry, which are: (i) an intermittent flow that passes from quiescent states to flaring activity, (ii) no quasi-steady-state jet, (iii) no possibility of a magnetically arrested configuration. Moreover, a further distinctive feature of this geometry is the intense magnetic reconnection events, occurring as layers of opposite magnetic polarity, accreted in the vicinity of the black hole. Finally, we argue that the absence of a jet structure in such case will be a smoking gun in 43 and 86 GHz observations.