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Milky Way dwarf satellites are unique objects that encode the early structureformation and therefore represent a window into the high redshift Universe. Sofar, their study was conducted using electromagnetic waves only. The futureLaser Interferometer Space Antenna (LISA) has the potential to reveal Milky Waysatellites in gravitational waves emitted by double white dwarf (DWD) binaries.We investigate gravitational wave (GW) signals detectable by LISA as a possibletool for the identification and characterisation of the Milky Way satellites.We use the binary population synthesis technique to model the population ofDWDs in dwarf satellites and we assess the impact on the number of LISAdetections when making changes to the total stellar mass, distance, starformation history and metallicity of satellites. We calibrate predictions forthe known Milky Way satellites on their observed properties. We find that DWDsemitting at frequencies $\gtrsim 3\,$mHz can be detected in Milky Waysatellites at large galactocentric distances. The number of these highfrequency DWDs per satellite primarily depends on its mass, distance, age andstar formation history, and only mildly depends on the other assumptionsregarding their evolution such as metallicity. We find that dwarf galaxies with$M_\star>10^6\,$M$_{\odot}$ can host detectable LISA sources with a number ofdetections that scales linearly with the satellite's mass. We forecast that outof the known satellites, Sagittarius, Fornax, Sculptor and the MagellanicClouds can be detected with LISA. As an all-sky survey that does not sufferfrom contamination and dust extinction, LISA will provide observations of theMilky Way and dwarf satellites galaxies valuable for Galactic archaeology andnear-field cosmology.

Populations of double white dwarfs in Milky Way satellites and their detectability with LISA