An extremely small and dense neutron star of mass M, and radius. R is rotating at an angular frequency $\mathrm{\omega }$. If an object is placed at its equator, it will remain stuck to it due to gravity if

• A

  $\mathrm{M}>\frac{\mathrm{R\omega }}{\mathrm{G}}$

• B

  $\mathrm{M}>\frac{{\mathrm{R}}^2{\mathrm{\omega }}^2}{\mathrm{G}}$

• C

  $\mathrm{M}>\frac{\mathrm{R\omega }}{{\mathrm{G}}^2}$

• D

  $\mathrm{M}>\frac{{\mathrm{R}}^3{\mathrm{\omega }}^2}{\mathrm{G}}$