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Single star evolution does not allow extremely low-mass stars to cross theclassical instability strip (IS) during the Hubble time. However, within binaryevolution framework low-mass stars can appear inside the IS once the masstransfer (MT) is taken into account. Triggered by a discovery of low-mass 0.26Msun RR Lyrae-like variable in a binary system, OGLE-BLG-RRLYR-02792, weinvestigate the occurrence of similar binary components in the IS, which set upa new class of low-mass pulsators. They are referred to as Binary EvolutionPulsators (BEPs) to underline the interaction between components, which iscrucial for substantial mass loss prior to the IS entrance. We simulate apopulation of 500 000 metal-rich binaries and report that 28 143 components ofbinary systems experience severe MT (loosing up to 90% of mass), followed by atleast one IS crossing in luminosity range of RR Lyrae (RRL) or Cepheidvariables. A half of these systems enter the IS before the age of 4 Gyr. BEPsdisplay a variety of physical and orbital parameters, with the most importantbeing the BEP mass in range 0.2-0.8 Msun, and the orbital period in range10-2500 d. Based on the light curve only, BEPs can be misclassified as genuineclassical pulsators, and as such they would contaminate genuine RRL andclassical Cepheid variables at levels of 0.8% and 5%, respectively. We statethat the majority of BEPs will remain undetected and we discuss relevantdetection limitations.

The occurrence of Binary Evolution Pulsators in the classical instability strip of RR Lyrae and Cepheid variables