Advertisement

Lunar Occultation Measurements of Stellar Angular Diameters

  • A. Richichi
Conference paper
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUS, volume 189)

Abstract

Offering an angular resolution which has remained unattained by any other technique for decades, lunar occultations have traditionally been the most productive method for the measurement of stellar angular diameters. Unlike interferometric methods, which are limited in resolution by the size of the aperture or of the baseline between apertures, in a lunar occultation the key to high angular resolution is the phenomenon of diffraction by a straight edge, that occurs at the Moon’s limb in a turbulence-free environment. For the reader not familiar with the physics and technical aspects of the lunar occultation (LO) technique, it is sufficient here to show in Fig. 1 some practical examples of occultation lightcurves for sources with different angular diameters. It can be noted that the contrast of the fringes is maximum for a point-like source; it then decreases with the angular diameter, and eventually reaches the regime of a monotonic drop in the signal -as predicted by simple geometrical optics-when the angular extent of the source is large. In practice, the LO method is well suited to measure angular diameters in the range 1 to 50 milliarcseconds (mas). There is no real limitation concerning the wavelength of observation, although at present the near-IR is the region of choice for several different reasons (Richichi 1994).

Keywords

Spectral Type Angular Diameter High Angular Resolution Carbon Star Interferometric Method 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Di Benedetto, G.P., Rabbia, Y. (1987), A&A, 188, 114ADSGoogle Scholar
  2. Dyck, H.M., Benson, J.A., van Belle, G.T., Ridgway, S.T. (1996), AJ, 111, 1705ADSCrossRefGoogle Scholar
  3. Perrin, G., Coude du Foresto, V., Ridgway, S.T., Mariotti, J.-M. (1996), these proceedings.Google Scholar
  4. Richichi, A. (1994), IAU Symposium 158 Very High Angular Resolution Imaging, Tango, W.J., Robertson, J.G. (eds.), p. 71CrossRefGoogle Scholar
  5. Richichi, A., Gaffa, C., Calamai, G., Lisi, F. (1996), AJ, 112, 2786ADSCrossRefGoogle Scholar
  6. Stecklum, B., Käufl, U., Richichi, A. (1996), ESO Workshop Science with the VLT Interferometer, Paresce, F. (ed.)Google Scholar
  7. Ridgway S.T., Joyce, R.R., White, N.M., Wing, R.F. (1980), ApJ, 235, 126ADSCrossRefGoogle Scholar
  8. White, N.M., Feierman, B.H. (1987), AJ, 94, 751ADSCrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1997

Authors and Affiliations

  • A. Richichi
    • 1
  1. 1.Osservatorio Astrofisico di Arcetri Largo E. FermiFirenzeItaly

Personalised recommendations