Lunar Occultation Measurements of Stellar Angular Diameters

Author(s):  
A. Richichi
1986 ◽  
Vol 91 ◽  
pp. 961 ◽  
Author(s):  
P. C. Schmidtke ◽  
J. L. Africano ◽  
G. H. Jacoby ◽  
R. R. Joyce ◽  
S. T. Ridgway

1980 ◽  
Vol 85 ◽  
pp. 1496 ◽  
Author(s):  
S. T. Ridgway ◽  
G. H. Jacoby ◽  
R. R. Joyce ◽  
D. C. Wells

1979 ◽  
Vol 50 ◽  
pp. 6-1-6-14 ◽  
Author(s):  
Stephen T. Ridgway

AbstractThis review of the lunar occultation technique summarizes results of 94 diameter measurements for 62 stars. The range of angular diameters measured, the coverage of spectral types, and the wavelengths studied are illustrated and discussedo Comparison with other techniques, magnitude limits and possible future developments are also considered.


1977 ◽  
Vol 82 ◽  
pp. 414 ◽  
Author(s):  
S. T. Ridgway ◽  
D. C. Wells ◽  
R. R. Joyce

1997 ◽  
Vol 189 ◽  
pp. 45-50 ◽  
Author(s):  
A. Richichi

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).


1982 ◽  
Vol 87 ◽  
pp. 680 ◽  
Author(s):  
S. T. Ridgway ◽  
G. H. Jacoby ◽  
R. R. Joyce ◽  
M. J. Siegel ◽  
D. C. Wells

1987 ◽  
Vol 94 ◽  
pp. 751 ◽  
Author(s):  
Nathaniel M. White ◽  
Barry H. Feierman

1979 ◽  
Vol 84 ◽  
pp. 247 ◽  
Author(s):  
S. T. Ridgway ◽  
D. C. Wells ◽  
R. R. Joyce ◽  
R. G. Allen

1982 ◽  
Vol 87 ◽  
pp. 1044 ◽  
Author(s):  
S. T. Ridgway ◽  
G. H. Jacoby ◽  
R. R. Joyce ◽  
M. J. Siegel ◽  
D. C. Wells

1982 ◽  
Vol 87 ◽  
pp. 808 ◽  
Author(s):  
S. T. Ridgway ◽  
G. H. Jacoby ◽  
R. R. Joyce ◽  
M. J. Siegel ◽  
D. C. Wells

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