Abstract
Photoelectric observations of the eclipsing binary IQ Persei have been carried out in B and V colours at Ege University Observatory. The corresponding light curves were analyzed by synthesis techniques. The absolute physical parameters and apsidal motion period (122 yr) of the system were obtained. The results have been compared with theoretical evolutionary models which include both mass loss and convective overshooting. Theoretical evolutionary tracks of the component stars indicate an age of 1.3 × 108 years and an apsidal motion constant of 0.0040 which is greater than its observed value by only about 5%. The A7 secondary of the eclipsing pair is still close to the zero-age main sequence but B7 primary is about halfway through its main sequence life-time.
Similar content being viewed by others
References
Burke, E.W., Jr.: 1968, IAU Inf. Bull. Variable Stars, No. 269.
Claret, A. and Gimenez, A.: 1991, Astron. Astrophys. Suppl. Ser. 87, 507.
Cowling, T.G.: 1938, Mon. Not. R. Astron. Soc. 98, 734.
Devlen, A.: 1995, unpublished M.Sc. thesis.
Drozdz, M., Krzesinski, J. and Pajdosz, G.: 1990, IAU Inf. Bull. Variable Stars, No. 3494.
Etzel, P.B. and Wood, D.B.: 1982, WINK Status Report, No. 10 (private communication).
Grygar, J., Cooper, M.L. and Jurkevich, I.: 1972, Bull. Astron. Inst. Czech. 23, 147.
Hall, D.S., Gertken, R.H. and Burke, E.W., Jr.: 1970, Publ. Astron. Soc. Pac. 82, 1077.
Hejlesen, P.M.: 1980, Astron. Astrophys. Suppl. Ser. 39, 347.
Hejlesen, P.M.: 1987, Astron. Astrophys. Suppl. Ser. 69, 251.
Hoffmeister, C.: 1949, Astr. Abh. Erg. Astr. Nach. 12(1), A21.
Lacy, C.H. and Frueh, M.L.: 1985, Astrophys. J. 295, 569.
Martynov, D.Ya.: 1971, in: V.P. Tsesevich (ed.), Zatmennyje Peremennye zvezdy, Moscow, p. 325.
Meisel, D.D.: 1968, Astron. J. 73, 350.
Popper, D.M.: 1980, Annu. Rev. Astron. Astrophys. 18, 115.
Russell, H.N.: 1928, Mon. Not. R. Astron. Soc. 88, 641.
Schwarzschild, M.: 1958, Structure and Evolution of the Stars, Dover, New York.
Shen, L.Z.: 1988, in: K.C. Leung (ed.), Critical Observations Versus Physical Models For Close Binary Systems, p. 239.
Smith, R.C.: 1983, The Observatory 103, 29.
Sterne, T.E.: 1939, Mon. Not. R. Astron. Soc. 99, 451.
Swings, P.: 1936, Z. Astrophys. 12, 40.
Wood, D.B.: 1971, Astron. J. 76, 701.
Wood, D.B.: 1972, A Computer Program for Modeling Non-Spherical Eclipsing Binary Star Systems, Goddard Space Flight Center, Greenbelt, Maryland, U.S.A.
Wood, D.B.: 1973–1978, WINK Status Reports, No. 1–9 (private communication).
Wilson, R.E.: 1979, Astrophys. J. 234, 1054.
Wilson, R.E.: 1990, Astrophys. J. 356, 613.
Wilson, R.E.: 1993, in: K.C. Leung and I.-S. Nha (eds.), in New Frontiers in Binary Star Research, ASP Conf. Ser. 38, ASP, San Francisco, p. 91.
Wilson, R.E.: 1994, private communication.
Wilson, R.E. and Devinney, E.J.: 1971, Astrophys. J. 166, 605.
Young, A.: 1975, Publ. Astron. Soc. Pac. 87, 717.
Zeipel, H., von: 1924, Mon. Not. R. Astron. Soc. 84, 665.
Rights and permissions
About this article
Cite this article
Değirmenci, ö. Photometry and Analysis of the Eclipsing Binary IQ Persei. Astrophysics and Space Science 253, 237–252 (1997). https://doi.org/10.1023/A:1000646708794
Issue Date:
DOI: https://doi.org/10.1023/A:1000646708794