Abstract
We consider a simple Newtonian model of a non-rotating white dwarf containing a dark-matter admixture. The baryonic component is described by the Chandrasekhar equation of state for acold degenerate electron gas, whereas the dark component is modeled as an independent polytropicfluid. The two components are coupled only through the common Newtonian gravitational field.Numerical solutions are constructed for a reference baryonic sequence and for representative mixedconfigurations with fixed dark-sector parameters. Attention is restricted to three basic outputs:the density profiles, the mass–radius relation, and the limiting mass readout within the exploreddensity interval. At ρb,c= 108g cm−3, the representative mixed models reduce the total mass byabout 14.08% for δ = 0.25 and by about 19.17% for δ = 0.35, relative to the purely baryonicconfiguration. The goal is not to identify a specific dark-matter particle model, but to provide atransparent baseline calculation showing how an additional gravitating component can modify theequilibrium sequence of white dwarfs.