Atmospheric dynamics and shock waves in RR Lyr

I. The three Hα emissions^★

¹ Observatoire de Haute-Provence – CNRS/PYTHEAS/Université d’Aix-Marseille, 04870 Saint Michel l’Observatoire, France
e-mail: denis.gillet@osupytheas.fr
² Observatoire d’Oukaïmeden, Faculté des Sciences et Techniques, Département de Physique, LPHEA, Marrakech, Morocco
e-mail: sefyani@uca.ma
³ Observatoire du Val de l’Arc, route de Peynier, 13530 Trets, France
e-mail: bma.ova@gmail.com
⁴ Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
⁵ Observatoire des Tourterelles, 34140 Mèze, France
⁶ Observatoire Canigou, route de Pau, 64445 Pau, France

Received: 4 July 2023
Accepted: 16 September 2023

Abstract

Context. Although spectroscopic observations of RR Lyrae stars have been underway for almost a century, the fact that the hydrogen line exhibits three successive emissions in each pulsation cycle is still a very recent discovery.

Aims. The purpose of the present study is to clarify the physical origin of these three emissions and their connection to atmospheric dynamics and to examine the influence of Blazhko modulation on their intensity.

Methods. We used 2437 high-resolution spectra over a total of 81 nights taken by the ELODIE spectrograph (Haute Provence Observatory, France) in the years 1994–1997, rounded out with a 2015 run from Oukaïmeden Observatory (Morocco). We performed a detailed analysis of the line profile variations over the whole pulsation cycle.

Results. Based on the blueshift of the main Hα emission, the velocity of the hypersonic shock front was estimated at between 100 and 150 ± 10 km s⁻¹ (Mach number between 10 and 15). It has been established that the shock velocity increases from the minimum Blazhko to its maximum and afterward, it gradually decreases to the Blazhko minimum to start growing again. This observational result is consistent with the shock model proposed in 2013 to explain the Blazhko effect. The intensity of the Hα emission increases with the shock velocity up to a maximum value around 137 km s⁻¹ and then decreases as the shock velocity increases further. This effect would be the consequence of the increasingly important ionization of the atoms in the radiative shock wake. The second (blueshifted) Hα emission is the consequence of an approximately constant supersonic compression (Mach number between 2 and 3) of the upper atmosphere falling onto the photospheric layers, during 3 to 16% of the pulsation period. Finally, the third Hα emission (P-Cygni profile) would be the consequence of the expansion of the high atmosphere induced by the shock wave during its final weakening.