All Tables

Table 1: Observed mean periods of the three detected oscillation frequencies with their corresponding mean amplitudes. The first two periods are reported by Rodriguez et al. (1992), and the third one is proposed by Pócs et al. (2002). The last column gives the frequency ratio f₁/f_i=2,3.
Table 2: Observed amplitudes and phases (referred to y) and their corresponding uncertainties in the four filters of the Strömgren system.
Table 3: Main characteristics of computed models representative of RV Ari. Labels ranging from 0 to 4 indicate the location of the models in the HR diagram displayed in Fig. 1. From left to right, M represents the stellar mass in solar masses ${{M}_{\odot }}$ ; $T_{{\rm eff}}$ the effective temperature in K (on a logarithmic scale); g the surface gravity in cgs (on a logarithmic scale); $X_{{\rm c}}$ the central hydrogen mass fraction; the age in Myr; $\alpha$ the mixing-length parameter; $\nu _{{\rm min}}$ - $\nu _{{\rm max}}$ represents the frequency range ( $\mu {\rm Hz}$ ) of predicted unstable modes; $\Delta z/H_p$ the size of the external convective zone normalised by the local pressure scaleheight measured at the bottom of the convection zone; $\Delta z/R_*$ the fraction of stellar radius occupied by the external convective zone; $\nu _{{\rm f}}$ the fundamental radial mode (in $\mu {\rm Hz}$ ); and finally, $\bar \rho$ represents the stellar mean density (in cgs).
Table 4: Main characteristics of computed models representative of RV Ari for the two rotational velocities considered. Labels i from 0 to 4 indicate the location of the models in the HR diagram given in Fig. 1. From left to right, $\Omega$ represents the rotational velocity in $\rm{km}~\rm{s}^{-1}$ , M the stellar mass in solar masses ${{M}_{\odot }}$ , $T_{{\rm eff}}$ the effective temperature in K (on a logarithmic scale), g the surface gravity in cgs (on a logarithmic scale), $X_{{\rm c}}$ the central Hydrogen fraction, the age in Myr, $\nu _{{\rm f}}$ the frequency of the fundamental radial mode (in $\mu {\rm Hz}$ ), and finally, $\nu _\Omega$ represents the rotational frequency (in $\mu {\rm Hz}$ ) of the model.
Table 5: Coupled modes found for the i2 models with $\Omega=52.6~\rm {km}~\rm {s}^{-1}$ (see Table 4). The mode identification is given by its radial order n, spherical degree $\ell$ , and azimuthal order m. $\sigma _a$ and $\sigma _b$ (in $\mu {\rm Hz}$ ) represent the oscillation frequency. $\beta _j$ is the contamination coefficient (see text for definition).
Table 6: Compilation of the most restrictive ranges of physical parameters obtained in the present work for RV Ari. The first line corresponds to the results obtained using non-rotating, non-adiabatic models, and the second line shows results from using rotating, adiabatic models.