Speckle interferometry of the spectroscopic binary 17 XI Cephei A

Details Speckle interferometry of the spectroscopic binary 17 XI Cephei A Speckle interferometry of the spectroscopic binary 17 XI Cephei A

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..522m&link_type=abstract

Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 522-525.

Astronomy and Astrophysics

Astrophysics

10

Astronomical Spectroscopy, Binary Stars, Interferometry, Speckle Patterns, Stellar Spectra, Orbital Elements, Stellar Luminosity, Stellar Mass

Scientific paper

Speckle interferometric observations with the 4 m Mayall telescope of the double-lined spectroscopic binary 17 ζ Cephei A are analyzed to determine the visual orbit of the system. Ten observations of angular separation and position angle yield the elements: P = 2.254 ± 0.005 yr, T = 1975.480 ± 0.005, e = 0.589 ± 0 010 α" = 0".073 ± 0".002 i = 71?9 ± 1°.0, and Ω = 93°.5 ± 1°.0. The speckle observations have rms residuals in both X and Y of ∼0".0022. Adoption of the spectroscopic mass ratio 2.8 ± 0.2 of Vickers and Scarfe and a distance of 33 ± 3 pc based on the spectroscopic parallax of the F7 V component ξ Cep B leads to MAa = 2.05 ± 0.64 Msun, MAb = 0.74 ± 0.23 Msun, MV Aa = 2.5 ± 0.2 mag, and Mv Ab = 2.8 ± 0.2 mag. The secondary is undermassive for its luminosity.

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