This abstract is primarily based on my recent paper ApJ 896, 69 (2020) along with MNRAS 490, 2692 (2019).
Over the past decades, various researchers have indirectly predicted at least a dozen of super-Chandrasekhar white dwarfs (white dwarfs which violate the Chandrasekhar mass-limit) from the luminosity observations of type Ia supernovae (SNeIa). Of course, there is no direct observations of super-Chandrasekhar white dwarfs so far. As a result, several research groups around the world proposed different models to explain the massive white dwarfs. Among them, the model for increasing mass accounting the presence of magnetic fields and rotation is the most popular one. In my presentation, I will explain that if such white dwarfs are rotating with a specific angular frequency following certain conditions, they can efficiently emit continuous gravitational waves, and these gravitational waves can be detected by various futuristic detectors, such as LISA, BBO, DECIGO, Einstein Telescope, etc., with a significant signal-to-noise ratio. I will also discuss various timescales over which these white dwarfs can emit dipole and quadrupole radiation, and the corresponding time required to obtain the optimum signal-to-noise ratio. In this way, in the future, we can detect the super-Chandrasekhar white dwarfs directly, and thereby can enforce better constraints in the theory of gravity to explain all the white dwarfs simultaneously.