  In this work, we study the impact of asymmetric dark matter (ADM) on low-mass
main-sequence stars in the Milky Way's nuclear star cluster, where the dark
matter (DM) density is expected to be orders of magnitude above what is found
near the Sun (${\rho }_{\mathrm{DM}}\gtrsim {10}^{3}\ \mathrm{GeV}\
{\mathrm{cm}}^{-3}$). Using a modified stellar evolution code and considering a
DM particle ($m_{\chi} = 4 \text{ GeV}$) with a spin-dependent interaction
cross section close to the limits allowed by direct detection, we found that
the interactions of ADM with baryons in the star's core can have two separate
effects on the evolution of these stars: a decrease in the hydrogen burning
rate, extending the duration of the main-sequence of stars with $M ~
1M_{\odot}$ by a few Gyr; the suppression of the onset of convection in the
core of stars with $M \lesssim 1.5M_{\odot}$ and consequent quench of supply
for the nuclear reactions. If we consider $\rho_{\text{DM}} > 10^3 \ \text{GeV
cm}^{-3}$ (corresponding to the inner 5 pc of the Milky Way), stars lighter
than the Sun will have a main-sequence life span comparable to the current age
of the universe. Stars heavier than two solar masses are not sensitive to the
DM particles considered here.

Solar and Stellar Astrophysics