  An ungravity-inspired model is employed to examine the astrophysical
parameters of white dwarf stars (WDs) using polytropic and degenerate gas
approaches. Based on the observed properties such as mass, radius, and
luminosity of selected WDs, namely, Sirius B and $\epsilon$ Reticulum, bounds
on the characteristic length and scaling dimension of the ungravity (UG) model
are estimated. The UG effect on the Chandrasekhar limit for WDs is shown. The
UG model is examined in the study of ultra-massive WDs, e.g., EUVE J1746-706.
In the contact of UG inspired model, a new location for some WDs on the
Hertzsprung-Russell diagram is found.
