Mozurkewich, D.,Johnston, K.J., Simon, R.S., Bowers, P.F., Gaume, R.A., Hutter, D.J., Colavita,M.M., Shao, M., & Pan X.-P. McAlister, H.A.1985, in Calibration of Fundamental Stellar Quantities, IAU Symp. Hutter, D.J.1994, in Amplitude and Intensity Spatial Interferometry II, SPIE Proc. II, Quirrenbach, A., Buscher, D.F.,Armstrong,J.T., Johnston, K.J., Simon, R.S., & Hutter, D.J. Hummel, C.A.,Mozurkewich, D., Elias, N.M. Hummel, C.A.,Armstrong, J.T., Quirrenbach, A., Buscher, D.F., Mozurkewich, D., Elias, N.M.II, & Wilson, R.E. Hummel, C.A.,Armstrong, J.T., Quirrenbach, A., Buscher, D.F., Mozurkewich, D., Simon,R.S.,& Johnston, K.J. The orbiting telescope with the Double Interferometer for Visual Astrometry (DIVA) will obtain, apart from astrometry, low-resolution spectra (A/AA 20). Griffin, R.F.1992, in Complementary Approaches to Double and Multiple Star Research, IAUColloquium 135, ed. 1993, Third Catalogue of Nearby Stars (preliminary version),available on the Astronomical Data Center CD ROM 1993,in Very High Angular Resolution Imaging, IAU Symp. 1994,in Amplitude and Intensity Spatial Interferometry II, SPIE Proc. 152Ĭolavita, M.M.,Shao, M., Hines, B.E., Wallace, J.K., Gursel, Y., Malbet, F., Yu, J.W., Singh,H., Beichman, C.A., Pan X.-P., Nakajima, T., & Kulkarni, S.R. 1994, in Amplitude and IntensitySpatial Interferometry II, SPIE Proc. DAO, 17, 1Ĭarleton, N.P.,Traub, W.A., Lacasse, M.G., Nisenson, P., Pearlman, M.R., Reasenberg, R.D., Xu,X., Coldwell, C.M., Panasyuk, A., Benson, J.A., Papaliolios, C., Predmore, R.,Schloerb, F.P., Dyck, H.M., & Gibson, D.M. 62Īrmstrong, J.T.,Hummel, C.A., Quirrenbach, A., Buscher, D.F., Mozurkewich, D., Vivekanand, M.,Simon, R.S., Denison, C.S., Johnston, K.J., Pan X.-P., Shao, M., &Colavita, M.M. This process is experimental and the keywords may be updated as the learning algorithm improves.Īrmstrong J.T.1994, in Amplitude and Intensity Spatial Interferometry II, SPIE Proc. These keywords were added by machine and not by the authors. New interferometers now coming into operation will make it possible to measure fundamental parameters in dozens to hundreds of binary systems. Luminosity estimates based on combined visual interferometric observations and velocity curves are often more precise than those from more indirect methods based on estimates of T eff. Observations of double-lined spectroscopic binaries with current interferometers have already yielded some mass estimates with precisions rivaling those from fitting the light curves of eclipsing double-lined systems. Interferometers now nearing completion will extend these values to a ≳ 500 μas and σ a ~ 10 μas. Long-baseline optical interferometry has made it possible to measure the visual orbits of binary stars with major axes as small as 5 mas and errors of ≲ 100 μas.
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