Turbulence amplification in the atmosphere of pulsating stars: a first approach

Details Turbulence amplification in the atmosphere of pulsating stars: a first approach Turbulence amplification in the atmosphere of pulsating stars: a first approach

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...332..235g&link_type=abstract

Astronomy and Astrophysics, v.332, p.235-244 (1998)

Astronomy and Astrophysics

Astrophysics

11

Stars: Individual: Delta Cephei, Cepheids, Line: Profiles, Turbulence, Shock Waves

Scientific paper

This paper is devoted to the understanding of the ``missing temperature``, called microturbulence by the astrophysicists, which appears when we want to modelize the width of stellar line profiles. In the framework of the two limiting turbulent regimes called ``incompressible'' and ``pressure released'', and expecting that the dissipation is negligible (``rapid distortion'' or RDT case), it is shown that the turbulence amplification in the atmosphere of a radially pulsating star is not only due to the global compression of the atmosphere during the pulsation. Strong shock waves propagating from the deep atmosphere to the very low density layers also play a role in the turbulence variation, especially when they become very strong i.e., hypersonic. The predicted turbulence amplification induced by the global atmospheric compression is consistent with the solenodial RDT. For shocks, the predicted turbulence amplification in the ``pressure released'' regime is overestimated with respect to stellar observations when the compression rate becomes larger than 2 which corresponds to a limit Mach number near 2. Thus, when radiative effects take place, the present turbulence amplification theory breaks down. A new approach is required.

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