By A. Labeyrie
Over the last twenty years, optical stellar interferometry has develop into a tremendous software in astronomical investigations requiring spatial answer well past that of conventional telescopes. This e-book, first released in 2006, was once the 1st to be written at the topic. The authors supply a longer advent discussing easy actual and atmospheric optics, which establishes the framework essential to current the guidelines and perform of interferometry as utilized to the astronomical scene. They persist with with an summary of old, operational and deliberate interferometric observatories, and a variety of significant astrophysical discoveries made with them. ultimately, they current a few as-yet untested rules for tools either at the floor and in house that may let us picture information of planetary structures past our personal.
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Additional info for An Introduction to Optical Stellar Interferometry
Magie, W. F. (1935). A Source Book in Physics, New York: McGraw Hill. Paczynski, B. (1986). Astrophys. , 304, 1. , J. Ehlers and E. E. Falco (1992). Gravitational Lenses, Berlin: Springer. , M. Jaroszynski, B. , (2005). Astrophys. J, 628, L109. 1 Interference and diffraction Following the qualitative introduction in the previous chapter, we continue with a more detailed discussion of interference. When two or more waves arrive at a point from different sources, or from the same source by different routes, they can interfere.
In 2002 he originated the idea of writing a textbook about optical interferometric astronomy, with the feeling that this was becoming a mature technique and was already beginning to provide important astrophysical data. This book is the result, and is dedicated to his memory. As a young man, Peter chose the study of math and physics over becoming a professional cello player but continued a life-long love of music. He was an avid Peter Nisenson, 1941–2004 xxxiii golf and tennis player and an active member of the Harvard College Observatory Tennis Club for years.
In principle, the larger the telescope aperture, the better is its inherent resolution. However, in practice, telescopes operating on the ground, observing through the Earth’s turbulent atmosphere, are limited by atmospheric turbulence. 1 2 Introduction The inherent or diffraction-limited angular resolution limit of a telescope is determined by the ratio λ/D between the wavelength, λ, of the light used for the observation and the diameter, D, of the telescope aperture. A 10-m telescope, like the Keck telescopes on Mauna Kea in Hawaii, has an inherent angular resolution limit of about 10 milli-arcseconds in visible light (λ = 500 nm).