Pulsational Characteristics of V1719 Cygni with Peculiar Light Curve

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Pulsating Star, Dwarf Cepheid, Metallicity

Scientific paper

The light curve and radial velocity curve of multiperiodic dwarf cepheid V1719 Cyg (HD200925) with peculiar light curve have been reanalysed in order to identify the oscillation modes to confirm the helium settling within the envelope. To do these, through the period search for the photometric and radial velocity data from the literature, two different periods were determined and the oscillation modes corresponding to the first and second periods were identified as the fundamental and first radial overtones. Hence the Helium settling within the enveloope was confirmed from the periodic ratio. The color excess, metallicity, effective temperature, and surface gravity corresponding to two different modes were determined and it was found that these parameters almost do not depend upon different oscillation mode. By utilizing the surface brightness method, we investigated the variation of angular diameter and radial displacement and it was found that angular variation is very peculiar. Also by referring to the stellar models, mass and age were determined as 2.7 Mo and 0.42 Gyr respectively which make this variable star heavier and younger than other multimode dwarf cepheids. Preliminary spectroscopic CCD observations were carried out and it was found that Mg in V1719 Cygni is nearly solar abundant according to the analysis of 5172.68A MgI line which is inconsistent with the photometric results. It was suggested that V1719 Cyg may be classified as a rho Pup stars according to the photometric characteristics

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