**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.
	ID	M	$T_{{\rm eff}}$	g	L	$X_{{\rm c}}$	Age	$\nu _{{\rm f}}$	$\nu _\Omega$
$\Omega=18$
	02	1.75	3.859	3.94	1.13	0.304	1182	130.85	1.8
	12	2.10	3.868	3.70	1.48	0.135	858	82.00	1.3
	22	2.00	3.850	3.70	1.39	0.126	994	82.26	1.3
	32	1.57	3.867	4.19	0.86	0.542	834	208.33	2.5
	42	1.49	3.850	4.20	0.76	0.554	920	202.46	2.6
$\Omega=52.6$
	02	1.76	3.859	3.94	1.14	0.305	1162	129.09	5.2
	12	2.10	3.868	3.70	1.48	0.141	854	82.18	3.6
	22	2.01	3.850	3.69	1.40	0.127	980	81.36	3.7
	32	1.58	3.868	4.19	0.87	0.543	815	210.00	7.3
	42	1.49	3.850	4.20	0.76	0.560	890	203.33	7.6

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