New techniques for determining sizes of satellites and asteroids.
It is pointed out that until very recently not even a crude idea of the sizes was available for any but the five brightest satellites and, more marginally, the three brightest asteroids. Attention is given to three new techniques which are yielding radii for dozens of small objects and which, by virtue of their independence of angular size, are capable of extension to even smaller and fainter objects. The first new technique, and by far the most precise, is to derive the radius, and in many cases the shape as well, from timings of an occultation of a star by the small body. Both of the other new techniques are based on methods of determining surface reflectivities, since once the geometric albedo is known, the radius can be determined from the brightness.