The asymmetry parameter M-m of the light curves of Cepheids in the Galaxy and Magellanic Clouds

Details The asymmetry parameter M-m of the light curves of Cepheids in the Galaxy and Magellanic Clouds The asymmetry parameter M-m of the light curves of Cepheids in the Galaxy and Magellanic Clouds

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...279..125a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 279, no. 1, p. 125-130

Mathematics

5

Cepheid Variables, Harmonics, Light Curve, Magellanic Clouds, Milky Way Galaxy, Stellar Models, Stellar Oscillations, Fourier Analysis, Limits (Mathematics), Maxima, Minima, Periodic Variations, Stellar Luminosity

Scientific paper

The parameter M-m (that is the interval between the phases of maximum M and minimum m of the light curve) of the population I Cepheids has been reconsidered. It is shown that the relation between M-m and P of the first overtone Cepheids in the MaAgellanic Clouds, which have a period range between approximately 1 and approximately 6 d, is similar to that observed in the corresponding galactic Cepheids, and this supports the hypothesis of the homogeneity of the group of first overtone Cepheids in the Galaxy, identified by means of Fourier parameters of the light curves. The use of synthetic light curves allows us to understand the trends and gaps observed in the (M-m) - P relation of fundamental mode Cepheids. The differences between these relations in the Galaxy and Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are discussed. A short discussion of the P - L relations and some speculations on the second overtone Cepheids are presented. Finally, stress is laid on the need of accurate light curves of Cepheids in external galaxies in order to get accurate values of the Fourier parameters and a better knowledge of the position of the resonance centers. These centers are of fundamental importance for the verification of the theories on stellar interior and evolution.

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