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Photometric observations from the last decade have revealed additionallow-amplitude periodicities in many classical pulsators that are likely due topulsations in non-radial modes. One group of multi-mode RR Lyrae stars, theso-called 0.61 stars, is particularly interesting. In these stars, the radialfirst overtone is accompanied by additional signals with period ratios around0.61. The most promising explanation for these signals is pulsation innon-radial modes of degrees 8 and 9. If the theory behind the additionalsignals in the 0.61 stars is substantiated, it would allow us to use non-radialmodes to study classical pulsators. We aim to perform asteroseismic modeling ofselected 0.61 stars with independently determined physical parameters to testwhether this assumption behind the modeling leads to correct results. Namely,we test whether the additional signals are indeed due to non-radial modes ofthe proposed moderate degrees. We selected a number of and RR Lyrae stars thatare also 0.61 stars and have good observational constraints on their otherphysical parameters. We assume that the nature of those modes is correctlyexplained with non-radial modes of degrees 8 or 9. Using this assumption andobservational constraints on physical parameters, we performed asteroseismicmodeling to test whether the observed periods and period ratios can bereproduced. For the majority of selected targets, we obtained a good matchbetween observed and calculated periods and period ratios. For a few targetshowever, the results obtained are ambiguous and not straightforward tointerpret.

Detailed asteroseismic modeling of RR Lyrae stars with non-radial modes