OHP Preprint No. 95 : Turbulence in RR Lyrae

Turbulence and broadening line phenomena in the variable star RR Lyrae

M. Chadid and D. Gillet

Observatoire de Haute-Provence (CNRS)
F-04870 Saint-Michel l'Observatoire, France
E-mail: chadid,gillet @obs-hp.fr

For the first time, the observation of three peaks within the FWHM curve of metallic absorption lines of a RR Lyrae pulsating star (RR Lyr) is clearly reported. A resolving power of 42,000 and a time resolution close to 1 of the pulsating period were necessary. We interpret the main peak (phase 0.926) mainly as a direct consequence of the line doubling phenomenon (Chadid and Gillet, 1996). At this phase, the occurrence of a turbulence increase needs to be quantified with a nonlinear, nonadiabatic pulsational model taking into account the propagation of strong shock waves. A second peak appears just after the luminosity maximum (phase 0.03) and is essentialy due to the rotation and pulsation without large turbulence contribution as for Cephei (Fokin, Gillet and Breitfellner 1996). The third peak occurs during the secondary acceleration (phase 0.70) and seems caused by the infalling shock ("early shock"). It induces a local overcompression during the atmospheric infalling ballistic motion and can certainly provoke a turbulence increase. Nevertheless, it is again necessary to compare our observations with a relevant theoretical model, to know if a shock turbulence amplification mechanism can give a significative contribution or if this amplification is only due to the global overcompression.

Keywords: Hydrodynamics -- Shock waves -- Stars: pulsation -- Stars: variables: RR Lyrae -- Stars: individual: RR Lyr

Astronomy&Astrophysics : Received 12 February 1996 / Accepted 7 May 1996
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