Abstract
By following the evolution of the stresses in a gravitating homogeneous planet during its accretion, it is possible to evaluate the differential stress in its interior if the compressibility and the rigidity of the substance are known functions of the density. The superficial layers are assumed to be in hydrostatic equilibrium. The radial pressure everywhere exceeds the horizontal pressures. The stress difference is null at the center of the planet, reaching its maximum at a depth of about one-third of the external radius. This value is roughly proportional to the fourth power of the external radius and inversely proportional to the superficial rigidity
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