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In the past decades, several neutron stars (NSs), particularly pulsars, withmass $M>2M_\odot$ have been observed. On the other hand, the existence ofmassive white dwarfs (WDs), even violating Chandrasekhar mass-limit, wasinferred from the peak luminosities of type Ia supernovae. Hence, there is ageneric question of the origin of massive compact objects. Here we explore theexistence of massive, magnetized, rotating NSs with soft and steep equation ofstates (EoSs) by solving axisymmetric stationary stellar equilibria in generalrelativity. For our purpose, we consider the Einstein equation solver forstellar structure XNS code. Such rotating NSs with magnetic field and rotationaxes misaligned, hence with non-zero obliquity angle, can emit continuousgravitational waves (GW), which can be detected by upcoming detectors, e.g.,Einstein Telescope, etc. We discuss the decays of magnetic field, angularvelocity and obliquity angle with time, due to angular momentum extraction byGW and dipole radiation, which determine the timescales related to the GWemission. Further, in the Alfv\'en timescale, a differentially rotating,massive proto-NS rapidly settles into an uniformly rotating, less massive NSdue to magnetic braking and viscosity. These explorations suggest thatdetecting massive NSs is challenging and sets a timescale for detection. Wecalculate the signal-to-noise ratio of GW emission, which confirms that anydetector cannot detect them immediately, but detectable by Einstein Telescopeand Cosmic Explorer over months of integration time, leading to directdetection of NSs.

Detection possibility of continuous gravitational waves from rotating magnetized neutron stars