  The Chandrasekhar limit for white dwarfs has been confirmed by many
astrophysical observations. However, how to obtain it theoretically in models
which rely on other-than-Heisenberg's uncertainty principles, which are
predicted by some quantum gravity theories, is not a trivial task. In this
manuscript, we will derive the Chandrasekhar mass assuming an uncertainty
relation proposed in the framework of Doubly Special Relativity, exhibiting
both a minimal length and a maximum momentum. We will show how to re-obtain an
asymptotically vanishing radius for the star in the limiting subcase of the
Heisenberg uncertainty principle: this is the same behavior as in the original
Chandrasekhar's derivation, but not when the more popular Generalized
Uncertainty Principle is assumed. We will argue that this is related to the
difference in the classical limit of these two different generalized
uncertainty principles, enlightening that the modified uncertainty parameter
considered here behaves like a finite temperature. The role of a maximum
momentum in guaranteeing the stability of the configuration, and in providing a
finite pressure for the degenerate electrons' gas, is also analyzed.
