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In order to shed light on the main physical processes controllingfragmentation of massive dense cores, we present a uniform study of the densitystructure of 19 massive dense cores, selected to be at similar evolutionarystages, for which their relative fragmentation level was assessed in a previouswork. We inferred the density structure of the 19 cores through a simultaneousfit of the radial intensity profiles at 450 and 850 micron (or 1.2 mm in twocases) and the Spectral Energy Distribution, assuming spherical symmetry andthat the density and temperature of the cores decrease with radius followingpower-laws. We find a weak (inverse) trend of fragmentation level and densitypower-law index, with steeper density profiles tending to show lowerfragmentation, and vice versa. In addition, we find a trend of fragmentationincreasing with density within a given radius, which arises from a combinationof flat density profile and high central density and is consistent with Jeansfragmentation. We considered the effects of rotational-to-gravitational energyratio, non-thermal velocity dispersion, and turbulence mode on the densitystructure of the cores, and found that compressive turbulence seems to yieldhigher central densities. Finally, a possible explanation for the origin ofcores with concentrated density profiles, which are the cores showing nofragmentation, could be related with a strong magnetic field, consistent withthe outcome of radiation magnetohydrodynamic simulations.

Fragmentation of massive dense cores down to ~1000 AU: Relation between fragmentation and density structure