An Introduction to Optical Stellar InterferometryDuring the last two decades, optical stellar interferometry has become an important tool in astronomical investigations requiring spatial resolution well beyond that of traditional telescopes. This book, first published in 2006, was the first to be written on the subject. The authors provide an extended introduction discussing basic physical and atmospheric optics, which establishes the framework necessary to present the ideas and practice of interferometry as applied to the astronomical scene. They follow with an overview of historical, operational and planned interferometric observatories, and a selection of important astrophysical discoveries made with them. Finally, they present some as-yet untested ideas for instruments both on the ground and in space which may allow us to image details of planetary systems beyond our own. |
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Table des matières
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Fig 86 a Typical design of a path equalizer using | 169 |
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Autres éditions - Tout afficher
An Introduction to Optical Stellar Interferometry A. Labeyrie,S. G. Lipson,P. Nisenson Aucun aperçu disponible - 2014 |
An Introduction to Optical Stellar Interferometry A. Labeyrie,S. G. Lipson,P. Nisenson Aucun aperçu disponible - 2006 |
Expressions et termes fréquents
adaptive optics amplitude angle angular diameter angular resolution aperture synthesis apodization array astrometry Astron astronomical Astrophys atmospheric autocorrelation axis baseline beam beam-combiner beam-splitter binary calculated camera coherence function combined configuration coronagraph correction correlation defined definition densified detection detector determined diffraction pattern disk dispersion distance example exo-Earths fibers field of view film find first fixed Fizeau flux focal Fourier transform Fraunhofer diffraction frequency Hanbury Brown hypertelescope infrared integrated intensity fluctuations intensity interferometry isoplanatic Labeyrie laser light limb darkening limit Lyot magnitude mask measured Michelson Michelson stellar interferometer mirror noise nonredundant nulling observed output pair path-length phase closure phase difference pinholes plane point spread function propagation pupil radius random reflected region result rotation separated shown in figure signal slits space spatial speckle image speckle interferometry speckle pattern spectral star stellar interferometer subapertures technique tip–tilt turbulence vector visible wave wavefront wavelength zero
Fréquemment cités
Page 3 - In general, the velocity depends on the relation between the density and the elasticity of the medium ; and the intensity is proportional to the square of the amplitude of the molecular vibrations.
Page 169 - ... boiling' of the image, closely resembling the appearances of objects viewed over a heated surface. "In the case of the two elements at opposite ends of a diameter of the objective, the same differences in phase produce a motion of the (straight) interference fringes (and not a confusion) and if. as is usually the case, this motion is not too rapid for the eye to follow, the visibility of the fringes is quite as good as In the case of perfect atmospheric conditions
Page 13 - This means that the power spectrum is the Fourier transform of the autocorrelation function (Wiener-Khinchin theorem).
Page 280 - Am., 36, 1667 (1966). [&] F. Lane, AIAA 5th Aerospace Science Meeting (New York, January 23-26, 1967). [9] AJ Favre, J. Appl. Mech., 241 (1965). [lO] RA Silverman, /. Appl.
Page 86 - The optical path is defined as the physical path multiplied by the refractive index of the medium in which it is propagating.
Informations bibliographiques
| Titre | An Introduction to Optical Stellar Interferometry |
| Auteurs | A. Labeyrie, S. G. Lipson, P. Nisenson |
| Éditeur | Cambridge University Press, 2006 |
| ISBN | 1139457683, 9781139457682 |
| Exporter la citation | BiBTeX EndNote RefMan |