Fourier analysis of the hydrodynamic models of classical Cepheids

Details Fourier analysis of the hydrodynamic models of classical Cepheids Fourier analysis of the hydrodynamic models of classical Cepheids

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...260..195f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 260, no. 1-2, p. 195-204.

Astronomy and Astrophysics

Astrophysics

7

Cepheid Variables, Fourier Analysis, Hydrodynamic Equations, Stellar Models, Stellar Oscillations, Helium Ions, Star Distribution

Scientific paper

Hydrodynamic models of classical Cepheids with pulsation periods from 3.7 to 32 d are calculated. The Fourier decomposition of the hydrodynamic solution has shown that for each Fourier harmonic of the velocity and radius, the temporal dependence is identified with a corresponding overtone. The kinetic energy and oscillatory moment of inertia are distributed among the overtones according to a power law, the spectrum being steeper with decreasing nonadiabaticity of the pulsation motions. The travelling pulse responsible for the energy transfer from the He(+) ionization zone into other layers of the envelope can be represented as a superposition of the overtones of order higher than the principal mode. At periods longer than 10 d, the secondary bump on the Cepheid light curves is due to the appearance at the surface of the outwardly moving pulse reflected off the stellar core. In Cepheids with periods from 6 to 9 d the secondary bump has another nature and is driven at the He(+) ionization zone by the second overtone. In Cepheids pulsating in the first overtone the Fourier harmonics of the order k is not less than 2 correspond to the even orders of the overtones.

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