CYCLE-TO-CYCLE CHANGES IN THE MIRA-TYPE STAR RT CYG

Автор(и)

  • V. I. Marsakova Department of Astronomy, Odessa State University, Україна
  • I. L. Andronov Department of Astronomy, Odessa State University, Україна

DOI:

https://doi.org/10.18524/1810-4215.1997.10.108189

Ключові слова:

Stars, Mira-type, RT Cyg

Анотація

RT Cyg was observed on photographic negatives of the Odessa plate collection. These data were reduced to the visual AFOEV system. The complete data set (n =7154) was studied by using several methods described by Andronov (l997b). 3-rd order trigonometric polynomial fit to the mean light curve corresponds to the period P= 190d.162 ± 0d.003 (coinciding with the value listed in GCVS (Kholopov et al., 1987) and asymmetry 0.458 (0.44 in GCVS). The characteristics of the cycles are determined and studied by using the correlation analysis.

Посилання

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Amdronov I.L.: 1997b, IAU Symp. 180 Planetary Nebulae, Kluwer Acad. Publ., 341.

Khopolov P.N. et all.: 1987, General Catalogue of Variable Stars; 4-th ed., 3, 368pp.

Marsakova V.I., Andronov L.L.: 1997, Kinemalilca Fizika. Neb. Tel, 13, N6, 49.

Schweitzer E.: 1993, Bull. AFOEV, 64, 14.

Strelkova E.P.: 1953, Izvestija Astron. Obs. Odessa State Univ, 3, 275.

Whittaker E., Robinson G.: 1926, The Calculus of Observations, Blackies & Sons, London.

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2017-08-01

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