We propose that when neutron stars in low-mass X-ray binaries accrete
sufficient mass and become millisecond pulsars, the interiors of these
stars may undergo phase transitions, exciting stellar radial oscillat
ions. We show that the radial oscillations will be mainly damped by gr
avitational-wave radiation instead of internal viscosity. Such gravita
tional waves may be detected by the advanced Laser Interferometer Grav
itational-wave Observatory.