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The Milky Way galaxy is estimated to be home to ten million to a billionstellar-mass black holes (BHs). Accurately determining this number anddistribution of BH masses can provide crucial information about the processesinvolved in BH formation, the possibility of the existence of primordial BHs,and interpreting gravitational wave (GW) signals detected in LIGO-VIRGO-KAGRA.Sahu et al. recently confirmed one isolated stellar-mass BH in our galaxy usingastrometric microlensing. This work proposes a novel method to identify suchBHs using the gravitational analog of the Gertsenshtein-Zel'dovich (GZ) effect.We explicitly demonstrate the generation of GWs when a kilohertz(kHz)electromagnetic (EM) pulse from a pulsar is intervened by a sphericallysymmetric compact object situated between the pulsar and Earth. Specifically,we show that the curvature of spacetime acts as the catalyst, akin to themagnetic field in the GZ effect. Using the covariant semi-tetrad formalism, wequantify the GW generated from the EM pulse through the Regge-Wheeler tensorand express the amplitude of the generated GW in terms of the EM energy andflux. We demonstrate how GW detectors can detect stellar-mass BHs byconsidering known pulsars within our galaxy. This approach has a distinctadvantage in detecting stellar mass BHs at larger distances since the GWamplitude falls as $1/r$.

Gertsenshtein-Zel'dovich gravitational analog can enable detection of solar mass black holes in Milky way galaxy