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Optical sensor design for advanced d...

Stanford University.

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Optical sensor design for advanced drag-free satellites.

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Optical sensor design for advanced drag-free satellites./
作者:	Allen, Graham Scott.
面頁冊數:	162 p.
附註:	Adviser: Robert L. Byer.
Contained By:	Dissertation Abstracts International70-07B.
標題:	Engineering, Aerospace. -
電子資源:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3364493
ISBN:	9781109242799

Optical sensor design for advanced drag-free satellites.
Allen, Graham Scott.

Optical sensor design for advanced drag-free satellites. - 162 p.

Adviser: Robert L. Byer.

Thesis (Ph.D.)--Stanford University, 2009.

The detection of gravitational waves in space uses the proof-mass of a drag-free satellite as an inertial reference. The Laser Interferometer Space Antenna (LISA) mission requires a drag-free proof-mass with residual acceleration noise less than 3x10-15m·s-1/ Hz and position sensing of 4x10-11 m/ Hz in a frequency band from 1 mHz to 1 Hz.

ISBN: 9781109242799Subjects--Topical Terms:

1018395
Engineering, Aerospace.

Optical sensor design for advanced drag-free satellites.
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502 $a Thesis (Ph.D.)--Stanford University, 2009.
520 $a The detection of gravitational waves in space uses the proof-mass of a drag-free satellite as an inertial reference. The Laser Interferometer Space Antenna (LISA) mission requires a drag-free proof-mass with residual acceleration noise less than 3x10-15m·s-1/ Hz and position sensing of 4x10-11 m/ Hz in a frequency band from 1 mHz to 1 Hz.
520 $a The Modular Gravitational Reference Sensor (MGRS) uses a single, optically sensed, spinning sphere as a drag-free reference. By eliminating the need for control forces and torques, we estimate the MGRS residual acceleration noise to be less than 9x10-16 m·s-2/ Hz , limited by direct disturbances to the proof-mass. We have developed a numeric simulation which demonstrates mass center position determination to better than 3 pm/ Hz limited by the performance of the individual optical sensors.
520 $a The Littrow grating cavity sensor is an experimental demonstration of a compact optical sensor designed to have a noise floor below 3 pm/ Hz . Using a Fabry-Perot cavity formed between a Littrow mounted diffraction grating and a reference surface, we have demonstrated a displacement noise of 10 pm/ Hz above 1 Hz. The sensor performance was limited by the laser frequency stability and could be reduced to below 1 pm/ Hz with a stabilized laser source.
520 $a This thesis establishes the foundations for the MGRS by investigating noise sources of the MGRS, data analysis techniques required to determine the mass center motion of a spinning sphere, and finally, the experimental demonstration of an optical sensor with displacement noise less than 10 pm/ Hz .
590 $a School code: 0212.
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650 4 $a Physics, Astronomy and Astrophysics. $3 1019521
650 4 $a Physics, Optics. $3 1018756
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