Gravitational Waves as Anisotropy of Space

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概要

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• A binary star system, which has a mutual orbiting rotational speed of ω_b, produces a time-dependent anisotropy of space at an observer. The equation of geodesic deviation shows that the resulting anisotropy of space gives rise to a gravitational force between two mirrors, which form an interferometer, and that force is proportional to ω^2_b times the anisotropy of space. Because 2π/ω_b is of the order of days or years, the rigidity k/m_o of the interferometer, where k is the force constant of a nongravitational force that supports the mirrors and m_o is the reduced mass of the mirrors, is much larger than ω^2_b. The amplitude of the vibrational motion of the interferometer with frequency ω_b (in terms of its equilibrium length) is given by (ω^2_b/(k/m_o)) times the anisotropy of space. On the other hand, if we rotate the interferometer with an angular speed of ω of 1 radian/s or more, we can make k/m_o<ω^2, in which case the factor (ω^2_b/(k/m_o)) disappears, and the rotating interferometer will be useful as a detector of the gravitational waves due to binary star systems. gravitational waves, binary star system, rotating interferometer, anisotropy of space

• 社団法人日本物理学会の論文
• 1993-12-15

著者

• MIZUSHIMA Masataka

  Department of Astrophysics, Nagoya University:(Present address) Department of Physics, University of Colorado

• Mizushima Masataka

  Department of Physics, University of Colorado

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