Abstract
Axial rotation of a star plays an important role in its evolution, physical condition in its atmosphere and appearance of its spectrum. Methods of determinations of υ sin i are based on comparison of the observed profiles of spectral lines with theoretical ones. Their accuracy depends on the kind and quality of spectrograms as well as on the algorithms used. A frequently used method is the simple comparing of one line, e.g. the Ca II at 3933 Å or Mg ii at 4481 Å. This however, may result in a false value of υ sin i if low dispersion spectra are used. In this work we studied contemporary CCD as well as older photographic spectra of the multiple star HD90569. We determined the projected rotational velocity value to be υ sin i = 11 km/s. Besides formerly reported enhancing of lines of Cr, Fe, Mn and Sr, we found also large overabundances of rare earths, gallium and platinum. Helium, carbon, nitrogen, oxygen, aluminium, calcium, scandium and nickel are in deficit. The spectrum of the occultation double was not identified to be of the SB2-type, however, there are some observable evidences that the pair creates a binary with a long orbital period. Despite this there are also observations that leave such interpretation uncertain.
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J. Zverko, J. Žižňovský, I. Iliev, et al., Astrophysical Bulletin 66, 325 (2011).
D. R. Palmer, E. N. Walker, D. H. P. Jones, and R. E. Wallis, R. Obs. Bull. 135, 385 (1968).
S. C. Wolff and G. W. Preston, Astrophys. J. Suppl. 37, 371 (1978).
F. Royer, J. Zorec, and A. E. Gomez, Astronom. and Astrophys. 463, 671 (2007).
H. A. Abt and N. I. Morrell, Astrophys. J. Suppl. 99, 135 (1995).
W. K. Bonsack, Publ. Astronom. Soc. Pacific 88, 19 (1976).
L. O. Lodén, J. Astroph. Astron. 8, 351 (1987).
C.R. Cowley and G. C. L. Aikman, Astrophys. J. 242, 684 (1980).
P. Renson and J. Manfroid, Astronom. and Astrophys. 498, 961 (2009).
S. J. Ademan, Astronom. and Astrophys. Suppl. Ser. 136, 379 (1999).
S. J. Adelman, Publ. Astronom. Soc. Pacific 118, 77 (2006).
M. Aurière, G. A. Wade, J. Silvester, et al., Astronom. and Astrophys. 475, 1053 (2007).
D. Hoffleit and J. H. Warren, Jr., The Bright Star Catalogue, 5th Revised Ed. (Astronomical Data Center, NSSDC/ADC, 1991).
W. I. Hartkopf and H. A. McAlister, Publ. Astronom. Soc. Pacific 96, 105 (1984).
H. A. Abt and M. S. Snowden, Astrophys. J. Suppl. 25 (1973).
V. Panchuk, V. Klochkova, M. Yushkin, and I. Najdenov, Journ. Opt. Technology 76, 87 (2009).
D. O. Kudryavtsev, Baltic Astron. 9, 649 (2000).
N. E. Piskunov and J. A. Valenti, Astronom. and Astrophys. 385, 1095 (2002).
P. Škoda, ASP Conf. Series 101, 187 (1996).
I. Hubeny, T. Lanz, and C. S. Jeffery, Newsletter on analysis of astronomical spectra No. 20 (1994).
J. Krtička, PhD Thesis, Masaryk University, Brno (1998) [in Czech].
F. Castelli and R. L. Kurucz, IAUS 210, A20 (2003).
N. E. Piskunov, F. Kupka, T. A. Ryabchikova, et al., Astronom. and Astrophys. Suppl. Ser. 112, 525 (1995).
T. A. Ryabchikova, N. E. Piskunov, F. Kupka, and W.W. Weiss, Baltic Astronomy 6, 244 (1997).
F. Kupka, N. E. Piskunov, T. A. Ryabchikova, et al., Astronom. and Astrophys. Suppl. Ser. 138, 119 (1999).
F. Kupka, T. A. Ryabchikova, N. E. Piskunov, et al., Baltic Astronomy 9, 590 (2000).
T. Moon and M.M. Dworetsky, Monthly Notices Roy. Astronom. Soc. 217, 782 (1985).
B. Smalley and M. M. Dworetsky, Astronom. and Astrophys. 293, 446 (1995).
J. Zverko, J. Žižňovský, Z. Mikulášek, and I. Kh. Iliev, Contrib. Astron. Obs. Skalnaté Pleso 37, 49 (2007).
D. Pourbaix, A. A. Tokovinin, A. H. Batten, et al., Astronom. and Astrophys. 424, 727 (2004).
F. Vansina and J. P. De Grève, Astrophys. and Space Sci. 87, 377 (1982).
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Original Russian Text © J. Zverko, I. Iliev, I. Romanyuk, I. Barzova, D. Kudryavtsev, I. Stateva, E. Semenko, 2012, published in Astrofizicheskij Byulleten, 2012, Vol. 67, No. 1, pp. 61–70.
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Zverko, J., Iliev, I., Romanyuk, I. et al. Stars with discrepant υ sin i as derived from Ca II 3933 and Mg II 4481 Å lines. II. Multiple star HD 90569. Astrophys. Bull. 67, 57–66 (2012). https://doi.org/10.1134/S1990341312010051
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DOI: https://doi.org/10.1134/S1990341312010051