We present non-linear hydrodynamic pulsation models for OGLE-BLG-RRLYR-02792 - a 0.26 M-circle dot pulsator, component of the eclipsing binary system, analysed recently by Pietrzynski et al. The star's light and radial velocity curves mimic that of classical RR Lyrae stars, except for the bump in the middle of the ascending branch of the radial velocity curve. We show that the bump is caused by the 2: 1 resonance between the fundamental mode and the second overtone - the same mechanism that causes the Hertzsprung bump progression in classical Cepheids. The models allow us to constrain the parameters of the star, in particular to estimate its absolute luminosity (approximate to 33 L-circle dot) and effective temperature (approximate to 6970 K, close to the blue edge of the instability strip). We conduct a model survey for the new class of low-mass pulsators similar to OGLE-BLG-RRLYR-02792 - products of evolution in the binary systems. We compute a grid of models with masses corresponding to half (or less) of the typical mass of RR Lyrae variable, 0.20 <= M <= 0.30 M-circle dot, and discuss the properties of the resulting light and radial velocity curves. Resonant bump progression is clear and may be used to distinguish such stars from classical RR Lyrae stars. We present the Fourier decomposition parameters for the modelled light and radial velocity curves. The expected values of the phi(31) Fourier phase for the light curves differ significantly from that observed in RR Lyrae stars, which is another discriminant of the new class.
Pulsation models for the 0.26 M-circle dot star mimicking RR Lyrae pulsator. Model survey for the new class of variable stars
PRADA MORONI, PIER GIORGIO;
2013-01-01
Abstract
We present non-linear hydrodynamic pulsation models for OGLE-BLG-RRLYR-02792 - a 0.26 M-circle dot pulsator, component of the eclipsing binary system, analysed recently by Pietrzynski et al. The star's light and radial velocity curves mimic that of classical RR Lyrae stars, except for the bump in the middle of the ascending branch of the radial velocity curve. We show that the bump is caused by the 2: 1 resonance between the fundamental mode and the second overtone - the same mechanism that causes the Hertzsprung bump progression in classical Cepheids. The models allow us to constrain the parameters of the star, in particular to estimate its absolute luminosity (approximate to 33 L-circle dot) and effective temperature (approximate to 6970 K, close to the blue edge of the instability strip). We conduct a model survey for the new class of low-mass pulsators similar to OGLE-BLG-RRLYR-02792 - products of evolution in the binary systems. We compute a grid of models with masses corresponding to half (or less) of the typical mass of RR Lyrae variable, 0.20 <= M <= 0.30 M-circle dot, and discuss the properties of the resulting light and radial velocity curves. Resonant bump progression is clear and may be used to distinguish such stars from classical RR Lyrae stars. We present the Fourier decomposition parameters for the modelled light and radial velocity curves. The expected values of the phi(31) Fourier phase for the light curves differ significantly from that observed in RR Lyrae stars, which is another discriminant of the new class.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
