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X-ray emission from counterparts of historical classical novae (CNe) in ourGalaxy is studied. To this end, we use data from three SRG/eROSITA sky surveysin the hemisphere analyzed by the RU eROSITA consortium. Out of 309 historicalCNe, X-ray emission has been detected from 52 sources with 0.3-2.3 keVluminosities in the $\rm L_X\approx 10^{30}\sim 10^{34}$ erg/s range. Amongthem, two sources have supersoft spectra and are associated with the post-novasupersoft X-ray emission. Hardness of X-ray spectra of some of the remainingsources tentatively suggests that magnetized white dwarfs (WDs) may account forsome fraction of CN counterparts detected in X-rays. This hypothesis will befurther tested in the course of the following SRG/eROSITA sky surveys. The CNcounterparts represent a bona fide sample of accreting WDs with unstablehydrogen burning on their surface, while their X-ray luminosity in quiescenceis a reasonable proxy for the accretion rate in the binary system. Using thisfact, we have constructed the accretion rate distribution of WDs with unstablehydrogen burning and compared it with the accretion rate distribution of knownsteady supersoft X-ray sources in our Galaxy and nearby external galaxies.There is a pronounced dichotomy between these two distributions with the CNcounterparts and the steady supersoft sources occupying different domains alongthe mass accretion rate axis, in accordance with the predictions of the theoryof hydrogen burning on the WD surface.

X-ray observations of historical classical nova counterparts with eROSITA telescope aboard SRG orbital observatory during the all-sky survey