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More than two dozen soft gamma-ray repeaters (SGRs) and anomalous X-raypulsars (AXPs) have been detected so far. These are isolated compact objects.Many of them are either found to be associated with supernova remnants or theirsurface magnetic fields are directly measured, confirming that they are neutronstars (NSs). However, it has been argued that some SGRs and AXPs are highlymagnetized white dwarfs (WDs). Meanwhile, the existence of super-ChandrasekharWDs has remained to be a puzzle. However, not even a single such massive WD hasbeen observed directly. Moreover, some WD pulsars are detected inelectromagnetic surveys and some of their masses are still not confirmed. Herewe calculate the signal-to-noise ratio for all these objects, consideringdifferent magnetic field configurations and thereby estimate the required timefor their detection by various gravitational wave (GW) detectors. For SGRs andAXPs, we show that, if these are NSs, they can hardly be detected by any of theGW detectors, while if they are WDs, Big Bang Observer (BBO), DECi-hertzInterferometer Gravitational wave Observatory (DECIGO) and Advanced LaserInterferometer Antenna (ALIA) would be able to detect them within a few days toa year of integration, depending on the magnetic field strength and itsconfiguration. Similarly, if a super-Chandrasekhar WD has a dominant toroidalfield, we show that even Laser Interferometer Space Antenna (LISA) and TianQinwould be able to detect it within one year of integration. We also discuss howGWs can confirm the masses of the WD pulsars.

Resolving dichotomy in compact objects through continuous gravitational waves observation