Peculiar double-periodic pulsation in RR Lyrae stars of the OGLE collection – II. Short-period stars with a dominant radial fundamental mode

• Published in: Monthly notices of the Royal Astronomical Society Vol. 465; no. 4; p. 4074
• Main Authors: Prudil, Z, Smolec, R, Skarka, M, Netzel, H
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 11.03.2017
• Subjects: Astronomy; Classification; Double stars; Fourier analysis; Frequency spectrum; Galactic bulge; Mathematical models; Modulation; Physical properties; Pulsation; Spectrum analysis; Stars
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stw3010

We report the discovery of a new group of double-periodic stars in the OGLE Galactic bulge photometry. In 38 stars identified as fundamental-mode RR Lyrae and four classified as first-overtone RR Lyrae, we detected an additional shorter periodicity. The periods of the dominant variability in the newly discovered group are 0.28 < P sub( D) < 0.41 d. Period ratios (0.68-0.72) are smaller than the period ratios of the Galactic bulge RRd stars. The typical amplitude ratio (of the additional to the dominant periodicity) is 20 per cent for the stars identified as fundamental-mode RR Lyrae and 50 per cent for stars classified as first-overtone RR Lyrae. 10 stars from our sample exhibit equidistant peaks in the frequency spectrum, which suggests the Blazhko-type modulation of the main pulsation frequency and/or additional periodicity. The Fourier coefficients R sub( 21) and R sub( 31) are some of the lowest among fundamental-mode RR Lyrae stars, but among the highest for the first-overtone pulsators. For the phase Fourier coefficients phi sub( 21) and phi sub( 31), our stars lie between RRab and RRc stars. The stars discussed were compared with radial linear pulsation models. Their position in the Petersen diagram cannot be reproduced by assuming that two radial modes are excited and their physical parameters are like those characteristic of RR Lyrae stars. The non-radial-mode scenario also faces difficulties. We conclude that the dominant variability is most likely due to pulsation in the radial fundamental mode, which applies to stars classified as first-overtone mode pulsators. At this point, we cannot explain the nature of the additional periodicity. Even more, the classification of the stars as RR Lyrae should be treated as tentative.