Expected frequency ( f ) and characteristic strain (h_c) of the GW signal produced by micro-TDEs involving an MS star (m_MS = 0.5 M_⊙, hatched bands) and a WD (m_WD = 1.4 M_⊙, solid coloured bands), shown at three reference distances:∼1 Mpc (red), ∼16 Mpc (blue), and z = 1 (grey). The two grey arrows in the lower-left corner indicate the directions of increasing BH mass (m_BH) and penetration factor (β ≡ r_t/r_p). These predictions are overlaid with the sensitivity curves of current and future GW detectors: LGWA (purple; Harms et al. 2021), LISA (sky blue; Amaro-Seoane et al. 2017), DECIGO (green; Sato et al. 2017), Kamioka Gravitational Wave Detector (KAGRA, gold; Abbott et al. 2021), the Einstein Telescope (ET, orange; Maggiore et al. 2020), the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO, violet; Abbott et al. 2017), and the Cosmic Explorer (CE, brown; Ng et al. 2021).