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We study the interaction of massless scalar fields with self-gravitatingneutron stars by means of fully dynamic numerical simulations of theEinstein-Klein-Gordon perfect fluid system. Our investigation is restricted tospherical symmetry and the neutron stars are approximated by relativisticpolytropes. Studying the nonlinear dynamics of isolated neutron stars is veryeffectively performed within the characteristic formulation of generalrelativity, in which the spacetime is foliated by a family of outgoing lightcones. We are able to compactify the entire spacetime on a computational gridand simultaneously impose natural radiative boundary conditions and extractaccurate radiative signals. We study the transfer of energy from the scalarfield to the fluid star. We find, in particular, that depending on thecompactness of the neutron star model, the scalar wave forces the neutron stareither to oscillate in its radial modes of pulsation or to undergogravitational collapse to a black hole on a dynamical timescale. The radiativesignal, read off at future null infinity, shows quasi-normal oscillationsbefore the setting of a late time power-law tail.Comment: 12 pages, 13 figures, submitted to Phys. Rev.

Scalar field induced oscillations of relativistic stars and gravitational collapse