Summary[edit]. Principe de l’interféromètre de Michelson Usage on ca. Usuari:Mcapdevila/Experiment de Michelson-Morley. interféromètre de Michelson. GeoGebra. Interféromètre Michelson. Author: helle. Angle. α = 45°. β = °. Boolean Value. Traces = true.

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The Michelson Interferometer has played an important role in studies of the upper atmosphererevealing temperatures and winds, employing both space-borne, and ground-based instruments, by measuring the Doppler widths and shifts in the spectra of airglow and aurora. More recently, the Helioseismic and Magnetic Imager HMIon the Solar Dynamics Observatoryemploys two Michelson Interferometers with a polarizer and other tunable elements, to study solar variability and to characterize the Sun’s interior along with the various components of magnetic activity.

Michelson interferometry is one leading method for the direct detection of gravitational waves.

File:Schéma d’un interféromètre de – Wikimedia Commons

The Michelson interferometer among other interferometer configurations is employed in many scientific experiments and became well known for its interferomwtre by Albert Michelson and Edward Morley in the famous Michelson-Morley experiment [1] in a configuration which would have detected the earth’s motion through the supposed luminiferous aether that most physicists at the time believed was the medium in which light waves propagated. This requirement can be met if both light paths cross an equal thickness of glass of the same dispersion.

The requirement for interferomette equalization is eliminated by interferometrf extremely narrowband light from a laser.

A sequence of phase-stepped images was processed to derive the wind velocity for two orthogonal view directions, yielding the horizontal wind vector. The null result of that experiment essentially disproved the existence of such an interferomehre, leading eventually to the special theory of relativity and the revolution in physics at the beginning of the twentieth century.


A convex spherical mirror is positioned so that its center of curvature coincides with the focus of the lens being tested.

File:Schéma d’un interféromètre de Michelson.PNG

The emergent beam is recorded by an imaging system for analysis. By using this site, you agree to the Terms of Use and Privacy Policy. To equalize the dispersion, a so-called compensating plate identical to the substrate of the beam splitter may be inserted into the path of the vertical beam. HMI takes high-resolution measurements of the longitudinal and vector magnetic field over the entire visible disk thus extending the capabilities of its predecessor, the SOHO ‘s MDI instrument See Fig.

Basics of Interferometry, Second Edition. Early experimentalists attempting to detect the earth’s velocity relative to the supposed luminiferous aethersuch as Michelson and Morley [1] and Miller[4] used quasi-monochromatic light only for initial alignment and coarse path equalization of the interferometer.

Another application is a sort of delay line interferometer that converts phase modulation into amplitude modulation in DWDM networks.

This led to the first polarizing wide-field Michelson interferometer described by Title and Ramsey [22] which was used for solar observations; and led to the development of a refined instrument applied to measurements of oscillations in the sun’s atmosphere, employing a network of observatories around the Earth known as the Global Oscillations Network Group GONG.

Each of those light beams is reflected back toward the beamsplitter which then combines their amplitudes using the superposition principle.

Retrieved 4 April White-light fringes were employed to facilitate observation of shifts in position of the interference pattern. Michelson pointed out that constraints on geometry forced by the limited coherence length required the use of a reference mirror of equal size to the test mirror, making the Twyman-Green impractical for many purposes. HMI observations will help establish the relationships between the internal dynamics and magnetic activity in order to understand solar variability and its effects.


Because the phase change from the Gires—Tournois etalon is an almost step-like function of wavelength, the resulting interferometer has special characteristics. American Journal of Physics.

File:Interferometre – Wikimedia Commons

Intrrferometre light from the tissue sample is combined with reflected light from the reference. Technology and Applications” PDF. The Michelson stellar interferometer is used for measuring the diameter of stars. If there is a slight angle between the two returning beams, for instance, then an imaging detector will record a sinusoidal fringe pattern as shown in Fig.

This is a Michelson interferometer in which the mirror in one arm is replaced with a Gires—Tournois etalon.

The unusual features of phase fluctuations in optical phase-conjugating mirror had been studied via Michelson interferometer with two independent PC-mirrors [33].

As seen in Fig.

Michelson interferometer

The characteristics of the interference pattern depend on intterferometre nature of the light source and the precise orientation of the mirrors and beam splitter. Views Read Edit View history. When using a noisy detector, such as at infrared wavelengths, this offers an increase in signal to noise ratio while using only a single detector element; 2 the interferometer does not require a limited aperture as do grating or prism spectrometers, which require the incoming light to pass through a narrow slit in order to achieve high spectral resolution.

In other projects Wikimedia Commons. The principle of using a polarizing Michelson Interferometer as a narrow band filter was first described by Evans [21] who developed a birefringent photometer where the incoming light is split into two orthogonally polarized components by a polarizing beam splitter, sandwiched between two halves of a Michelson cube. Retrieved 10 April