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The formation of subdwarf B (sdB) stars is not well understood within thecurrent framework of stellar single and binary evolution. In this study, wefocus on the formation and evolution of the pulsating sdB star in the veryshort-period eclipsing binary PG1336-018. We aim at refining the formationscenario of this unique system, so that it can be confronted with observations.We probe the stellar structure of the progenitors of sdB stars in short-periodbinaries using detailed stellar evolution calculations. Applying this toPG1336-018 we reconstruct the common-envelope phase during which the sdB starwas formed. The results are interpreted in terms of the standardcommon-envelope formalism (the alpha-formalism) based on the energy equation,and an alternative description (the gamma-formalism) using the angular momentumequation. We find that if the common-envelope evolution is described by thealpha-formalism, the sdB progenitor most likely experienced a helium flash. Wethen expect the sdB mass to be between 0.39 and 0.48 Msun, and the sdBprogenitor initial mass to be below ~2 Msun. However, the results for thegamma-formalism are less restrictive, and a broader sdB mass range (0.3 - 0.8Msun) is possible in this case. Future seismic mass determination will givestrong constraints on the formation of PG1336-018 and, in particular, on the CEphase.

An evolutionary study of the pulsating subdwarf B eclipsing binary PG1336-018 (NY Vir)