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Spectroscopic studies of Cepheids in Circinus (AV Cir, BP Cir) and Triangulum Australe (R TrA, S TrA, U TrA, LR TrA)

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Abstract

Based on high-resolution spectra taken with the 1.9-m telescope of the South African Astronomical Observatory, we have determined the atmospheric parameters and chemical composition for three small-amplitude (AV Cir, BP Cir, and LR TrA), two classical (R TrA and S TrA), and one double-mode (U TrA) Cepheids. The averaged atmospheric parameters have been estimated for three Cepheids (AV Cir, BP Cir, and U TrA) observed at various pulsation phases. In all Cepheids, except U TrA, the metallicity has turned out to be higher than the solar one by 0.1–0.2 dex. The abundances of the key elements of the evolution of yellow supergiants (C, O, Na, Mg, Al) show that these objects have already passed the first dredge-up, while those of the remaining elements are nearly solar. Comparison of our results on the Cepheids from the list (except U TrA) with those of other authors shows significant differences in C and O abundance estimates for AV Cir, R TrA, S TrA, and LR TrA. For AV Cir and BP Cir, the Hα line profiles are symmetric but with a slight asymmetry in the core at approximately the same phase near 0 P· 7: on the “blue” side for AV Cir and on the “red” one for BP Cir. BP Cir exhibits a distinct asymmetry in the absorption lines of neutral atoms and ions at various pulsation phases, which can be explained by nonradial first-overtone pulsations. The constancy of the Hα absorption line profiles with pulsation phase for AV Cir and BP Cir may suggest the presence of a hydrogen envelope around them. For the double-mode Cepheid U TrA, an asymmetry is observed in the cores of the Hα line and the absorption lines of neutral atoms and ions at various pulsation phases, which can be explained by nonradial pulsations in the Cepheid’s atmosphere. The absorption lines of neutral atoms and ions of metals in LR TrA closely resemble those in the well-known Cepheid BG Cru: secondary “blue” and “red” components whose line depths vary with pulsation phase are noticeable. This Cepheid can also pulsate in the first overtone and have an extended hydrogen envelope. Careful multiphase spectroscopic observations with a sufficiently high resolution are needed to test this assumption.

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Authors and Affiliations

  1. Astronomical Observatory, Odessa National University, Shevchenko park, Odessa, 65014, Ukraine

    I. A. Usenko

  2. South African Astronomical Observatory, P. O. Box 9, Observatory, Cape Town, 7935, South Africa

    A. Yu. Kniazev

  3. Southern African Large Telescope, P. O. Box 9, Observatory, Cape Town, 7935, South Africa

    A. Yu. Kniazev

  4. Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, Moscow, 119991, Russia

    A. Yu. Kniazev, L. N. Berdnikov & V. V. Kravtsov

  5. Departamento de Fisica, Facultad de Ciencias Naturales, Universidad de Atacama, Copayapu 485, Copiapo, Chile

    V. V. Kravtsov

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  1. I. A. Usenko
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  3. L. N. Berdnikov
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  4. V. V. Kravtsov
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Correspondence to I. A. Usenko.

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Original Russian Text © I.A. Usenko, A.Yu. Kniazev, L.N. Berdnikov, V.V. Kravtsov, 2014, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2014, Vol. 40, No. 12, pp. 857–877.

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Usenko, I.A., Kniazev, A.Y., Berdnikov, L.N. et al. Spectroscopic studies of Cepheids in Circinus (AV Cir, BP Cir) and Triangulum Australe (R TrA, S TrA, U TrA, LR TrA). Astron. Lett. 40, 800–820 (2014). https://doi.org/10.1134/S1063773714110061

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