The angular velocity of rotation of a star (of mass $M$ and radius $R$) at which the matter starts to escape from its equator will be:

  • A
    $\sqrt{\frac{2GM^2}{R}}$
  • B
    $\sqrt{\frac{2GM}{g}}$
  • C
    $\sqrt{\frac{2GM}{R^3}}$
  • D
    $\sqrt{\frac{2GR}{M}}$

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