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Direct Observations of the Heterogeneity of Supergiant Disks

  • J. W. Harvey (a1), C. R. Lynds (a1) and S. P. Worden (a2)

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Resolved images of the disks of the largest stars observed with the largest telescopes can be constructed using the class of techniques called speckle imaging. The observations must be made with narrow passbands (~ 10 nm), short exposures (~ 20 ms) compensation for atmospheric dispersion, high magnification and good signal-to-noise ratio. One specific technique applied to a Ori (Lynds et al., 1976) shows slight but apparently real differences in the images of the disk corresponding to low and high opacity in the stellar atmosphere which we interpret as due to temperature differences. There are also significant differences in the star’s diameter and/or limb darkening at the two different opacity wavelengths.

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References

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Lynds, C. R., Worden, S. P., and Harvey, J. W.: 1976, Astrophys. J. 207, 174.
McDonnell, M. J., and Bates, R. H. T.: 1976, Astrophys. J. 208, 443.
Nisenson, P., Elm, D. C., and Stachnik, R. V.: 1976, Proc. SPIE 75, 83.

Direct Observations of the Heterogeneity of Supergiant Disks

  • J. W. Harvey (a1), C. R. Lynds (a1) and S. P. Worden (a2)

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