Abstract
TheUBV photoelectric light curve of IW Per as an ellipsoidal variable was obtained and a number of spectrograms were taken with dispersion of 10 Å mm−1. New spectroscopic orbital elements are determined for this single-line spectroscopic binary to beK 1=99.3 km s−1, γ=0.2 km s−1,a sini=1.80R ⊙ andf(m)=0.093m ⊙. From analysis of the light curve, the geometric ellipticity coefficient of the distorted components is determined to beZ=0.037.
Applying the second-order theory of light variation due to distorted components (Kopal and Kitamura, 1968), the orbital inclination and fractional radius of the primary component can be deduced simultaneously to bei=63° andr 1=0.294. By takingm 1=2.0m ⊙ for the mass of the primary component with spectral type A5Vm, the mass of the secondary can be also deduced to bem 2=1.08m ⊙, which would correspond to a G0-type if it is a Main-Sequence star. These elements indicate that the system is a non-eclipsing detached close binary.
From intensity measurements of the lines Caii-K, Srii λ 4215 and Scii λ 4320 on twenty-eight good spectrograms taken at various phases, those intensities and the intensity ratio Sc/Sr are found to vary systematically with phase. From these variations the distribution of the local metallicity on the surface of the Am primary component is discussed in connection with the distribution of the local surface temperature.
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References
Abt, H. A.: 1965:Astrophys. J. 11, 429.
Abt, H. A. and Bidelman, W. P.: 1969,Astrophys. J. 158, 1091.
Abt, H. A. and Hudson, K. I.: 1971,Astrophys. J. 163, 333.
Allen, C. W.: 1973,Astrophysical Quantities (3rd ed.), Athlone Press, London.
Bertaud, C. and Floquet, M.: 1967,J. des Observateurs 50, 425.
Conti, P. S.: 1965,Astrophys. J. 142, 1594.
Cowley, A., Cowley, C., Jaschek, M. and Jaschek, C.: 1969,Astron. J. 74, 375.
Crawford, D. L., Barnes, J. V., Gibson, J., Golson, J. C., Perry, C. L. and Crawford, M. L.: 1972,Astron. Astrophys. Suppl. 5, 109.
Eggen, O. J.: 1976,Publ. Astron. Soc. Pacific 88, 402.
Harper, W. E.: 1927,Publ. Dom. Astrophys. Obs., Victoria 4, 39.
Harper, W. E.: 1935,Publ. Dom. Astrophys. Obs., Victoria 6, 214.
Hauck, B.: 1973,Astrophys. J. Suppl. 10, 385.
Hilditch, R. W. and Hill, G.: 1975,Monthly Notices Roy. Astron. Soc. 79, 101.
Hosokawa, Y.: 1957,Sci. Rep. Tohoku Univ., Series I, Vol. XL, No. 4.
Jaschek, M. and Jaschek, C.: 1960,Z. Astrophys. 50, 155.
Johansen, K. T. and Gyldenkerne, K.: 1970,Astrophys. J. Suppl. 1, 429.
Kitamura, M., Kim, T. and Kiyokawa, M.: 1976,Ann. Tokyo Astron. Obs. II 16, 22.
Kopal, Z. and Kitamura, M.: 1968, inAdvances Astron. Astrophys. (ed. Z. Kopal), Academic Press, New York,6, 125.
Kukarkin, B. V., Kholopov, P. N., Efremuv, Yu. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Fedorovich, V. P. and Frolov, M. S.: 1969,General Catalogue of Variable Stars, Astron. Council, Acad. Sci. U.S.S.R., Moscow.
Magalashvili, N. L., Kumsishvili, J. J. and Razmadse, N. a.: 1956,Bull. Abastumani Astrophys. Obs. 20, 11.
Osawa, K.: 1959,Astrophys. J. 130, 159.
Osawa, K. and Hata, S.: 1960,Ann. Tokyo Astron. Obs. VI 4, 148.
Plaskett, J. S., Harper, W. E., Young, R. K. and Plaskett, H. H.: 1919,Publ. Dom. Astrophys. Obs., Victoria 1, 163.
Russell, H. N. and Merrill, J. E.: 1952,Princeton Contr. No. 26.
Smith, M. A.: 1970,Astrophys. J. 161, 1181.
Smith, M. A.: 1971b,Astron. J. 76, 896.
Smith, M. A.: 1971b,Astron. Astrophys. 11, 325.
Smith, M. A.: 1972,Astron. Astroph. Suppl. 5, 81.
Strittmatter, P. A. and Sargent, W. L. W.: 1966,Astrophys. J. 145, 130.
Titus, J. and Morgan, W. W.: 1940,Astrophys. J. 92, 256.
von Zeipel, H.: 1924,Monthly Notices Roy. Astron. Soc. 84, 702.
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Kim, TH. The metallic-line close binary system IW persei. Astrophys Space Sci 68, 355–384 (1980). https://doi.org/10.1007/BF00639705
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DOI: https://doi.org/10.1007/BF00639705