LASER ~ •632nm

=0.632um

REFERENCE MIRRO R

ADJUSTABLE MIRRO R

PHOTO-TRANSISTOR

SAMPLE

XY TABLE

Schematic of modified Michelson-Morley in­t~rferometer. The beam splitter first divides the input beam into a reference and object beam and then re­combines the two beal11B at the photcrddector where the different J>lllh l~ngths produce a fringe patlem.

Figura 1.12- Interferômetro de Michelson.

Figura 1.13- Arranjo experimental de um Interferômetro de Michelson.

Figura 1.14- Interferômetro de Michelson em tecnologia MEMS.

generation

pulsed laser beam

detection

Lase~ generation and detection of ultrasonic waves. '·

Figura 1.15- Técnica de laser-ultrasound.

source

measured object

(a)

CCDcamera

reference mirro r

'~--------------------------------------~ (b)

Figura 1.16- llllerferometria com luz branca. a) Arranjo do interferômetro em óptica

volumétrica. b) Levantamento do perfi/lateral de uma moeda.

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LASER INTERFEROMETER GRA VITATIONAL-WA VE OBSERVATORY (LIGO)

T 21mt

t 2km

l

Figure 1. LIGO Observatories: Hanfol'd, \Vashington and Livingstou Louisiana

Left Arm

End Stati.on

Mid Station

Sckemati.c IayoutofLIGO Site at:Ha:nmrd, WA Q:nsta.llati.on at Livillgston, LA:has JW mid-stati.ons)

Rigkt Arm

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LASER INTERFEROMETER SPACE ANTENNA (LISA)

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The three LISA spacecraft will be placed in orbits that form a triangular formation with center 20° behind the Earth and side length 5 million km. (The figure showing the formation is not to scale.)

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Each LISA spacecraft contains two instruments. Each instrument includes a 30-centimeter-diameter telescope for transmission and reception of laser signals from another spacecraft. Each instrument also has an optical bench that contains interferometer optics. An inertial sensor is mounted at the center of each optical bench, containing a proof mass shielded from nongravitational disturbances anda capacitar plate arrangement for measuring the position of the spacecraft with respect to the proof mass. The interferometer measures changes in the distance between proof masses in the different spacecraft. The spacecraft is kept centered on the proof masses, based on the capacitive sensors.

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LIGO Interference

LIGO Prototype

END STATION

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