  The Milky Way galaxy is estimated to be home to ten million to a billion
stellar-mass black holes (BHs). Accurately determining this number and
distribution of BH masses can provide crucial information about the processes
involved 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 using
astrometric microlensing. This work proposes a novel method to identify such
BHs 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 spherically
symmetric compact object situated between the pulsar and Earth. Specifically,
we show that the curvature of spacetime acts as the catalyst, akin to the
magnetic field in the GZ effect. Using the covariant semi-tetrad formalism, we
quantify the GW generated from the EM pulse through the Regge-Wheeler tensor
and express the amplitude of the generated GW in terms of the EM energy and
flux. We demonstrate how GW detectors can detect stellar-mass BHs by
considering known pulsars within our galaxy. This approach has a distinct
advantage in detecting stellar mass BHs at larger distances since the GW
amplitude falls as $1/r$.
