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Prompted by the recent successful predictions of the internal dynamics ofAndromeda's satellite galaxies (McGaugh & Milgrom 2013a,b), we revisit theclassical Milky Way dwarf spheroidal satellites Draco, Sculptor, Sextans,Carina, and Fornax in the framework of Milgromian dynamics (MOND). We use forthe first time a Poisson solver with adaptive mesh refinement (AMR) in order toaccount simultaneously for the gravitational influence of the Milky Way and itssatellites. This allows to rigorously model the important external field effect(EFE) of Milgromian dynamics, which can reduce the effective accelerationsignificantly. We make predictions on the dynamical mass-to-light ratio(Mdyn/L) expected to be measured by an observer who assumes Newtonian dynamicsto be valid. We show that Milgromian dynamics predicts typical Mdyn/L ~ 10-50Msun/Lsun. The results for the most luminous ones, Fornax and Sculptor, agreewell with available velocity dispersion data. Moreover, the central power-lawslopes of the dynamical masses agree exceedingly well with values inferredobservationally from velocity dispersion measurements. The results for Sextans,Carina and Draco are low compared to usually quoted observational estimates, asalready pointed out by Angus (2008). For Milgromian dynamics to survive furtherobservational tests in these objects, one would thus need that either (a)previous observational findings based on velocity dispersion measurements haveoverestimated the dynamical mass due to, e.g., binaries and contaminantoutliers, (b) the satellites are not in virial equilibrium due to the Milky Waytidal field, or (c) the specific theory used here does not describe the EFEcorrectly (e.g., the EFE could be practically negligible in some othertheories), or a combination of (a)-(c).

A census of the expected properties of classical Milky Way dwarfs in Milgromian dynamics