THE IMPORTANCE OF PHASE IN NULLING INTERFEROMETRY AND A THREE-TELESCOPE CLOSURE-PHASE NULLING INTERFEROMETER CONCEPT

摘要

We discuss the theory of the Bracewell nulling interferometer and explicitly demonstrate that the phase of the "white light" null fringe is the same as the phase of the bright output from an ordinary stellar interferometer. As a consequence, a "closure phase" exists for a nulling interferometer with three or more telescopes. We calculate the phase offset as a function of baseline length for an Earth-like planet around the Sun at 10 pc, with a contrast ratio of 10~(-6) at 10 μm. The magnitude of the phase due to the planet is ～10~(-6) radians, assuming the star is at the phase center of the array. Although this is small, this phase may be observable in a three-telescope nulling interferometer that measures the closure phase. We propose a simple nonredundant three-telescope nulling interferometer that can perform this measurement. This configuration is expected to have improved characteristics compared to other nulling interferometer configurations, such as a relaxation of path length tolerances, through the use of the "ratio of wavelengths" technique, a closure phase, and better discrimination between extrasolar zodiacal dust and planets.