Advertisement

Astrophysical Bulletin

, Volume 63, Issue 4, pp 357–360 | Cite as

Independent estimate of the interstellar extinction toward FU Ori

  • A. S. Kravtsova
  • E. V. Malogolovets
  • S. A. Lamzin
Article

Abstract

Speckle-interferometric observations of FU Ori are performed with the 6-m telescope of the Special Astrophysical Observatory with 600/40 nm and 800/100 nm (central bandwidth/halfwidth) filters. The companion star FU Ori S that was recently discovered at λ >-1.25µm was recorded in observations with the λλ==800/100 nm filter. The positional parameters and magnitude difference of the companion in the filter considered are found to be θ = (163.9 ± 1.0)°, ρ = (0.493 ± 0.007)″, Δm = 3.96 ± 0.28. An analysis of the spectral energy distribution of the companion implies that for the extinction A V toward FU Ori to be greater than about 1.6 m , i.e., the minimum value required by the available models of the fuor, the spectral type of the companion star must be no later than K3. The reliability of this conclusion and the possible ways for obtaining more accurate estimates of A V are discussed.

PACS numbers

97.10.Gz 97.21.+a 

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. 1.
    G. H. Herbig, Vistas in Astron. 8, 109 (1966).CrossRefADSGoogle Scholar
  2. 2.
    G. H. Herbig, Astrophys. J. 217, 693 (1977).CrossRefADSGoogle Scholar
  3. 3.
    L. Hartmann and S. J. Kenyon, Annu. Rev. Astronom. Astrophys. 34, 207 (1996).CrossRefADSGoogle Scholar
  4. 4.
    G. H. Herbig, P. P. Petrov and R. Duemmler, Astrophys. J. 595, 384 (2003).CrossRefADSGoogle Scholar
  5. 5.
    S. L. Skinner, K. L. Briggs, and M. Güdel, Astrophys. J. 643, 995 (2006).CrossRefADSGoogle Scholar
  6. 6.
    A. S. Kravtsova, S. A. Lamzin, L. Errico, et al., Pis’ma Astronom. Zh. 33, 846 (2007).Google Scholar
  7. 7.
    H. Wang, D. Apai, Th. Henning, et al., Astrophys. J. 601, L83 (2004).CrossRefADSGoogle Scholar
  8. 8.
    B. Reipurth and C. Aspin, Astrophys. J. 608, L65 (2004).CrossRefADSGoogle Scholar
  9. 9.
    A.F. Maksimov, Yu. Yu. Balega, E. V. Malogovets, et al., in preparation.Google Scholar
  10. 10.
    A. Labeyrie, Astronom. and Astrophys. 6, 85 (1970).ADSGoogle Scholar
  11. 11.
    I. I. Balega, Y. Y. Balega, K.-H. Hofmann, et al., Astronom. and Astrophys. 385, 87 (2002).CrossRefADSGoogle Scholar
  12. 12.
    J. G. Walker, Opt. Acta 28, 735 (1981).Google Scholar
  13. 13.
    C. Clarke, G. Lodato, S. Y. Melnikov, et al., Monthly Notices Roy. Astronom. Soc. 361, 942 (2005).CrossRefADSGoogle Scholar
  14. 14.
    S. J. Kenyon and L. Hartmann, Astrophys. J. Suppl. 101, 117 (1995).CrossRefADSGoogle Scholar
  15. 15.
    R. C. Bless and B. D. Savage, Astrophys. J. 171, 293 (1972).CrossRefADSGoogle Scholar

Copyright information

© MAIK Nauka 2008

Authors and Affiliations

  • A. S. Kravtsova
    • 1
  • E. V. Malogolovets
    • 2
  • S. A. Lamzin
    • 1
  1. 1.Sternberg Astronomical InstituteMoscowRussia
  2. 2.Special Astrophysical ObservatoryRussian Academy of SciencesNizhnij ArkhyzRussia

Personalised recommendations