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Signatures of hadron-quark mixed phase in gravitational waves

Hajime Sotani1,*, Nobutoshi Yasutake1, Toshiki Maruyama2, and Toshitaka Tatsumi3

  • 1Division of Theoretical Astronomy, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
  • 2Advanced Science Research Center, Japan Atomic Energy Agency, Tokai, Ibaraki 319-1195, Japan
  • 3Department of Physics, Kyoto University, Kyoto 606-8502, Japan

  • *hajime.sotani@nao.ac.jp
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Phys. Rev. D 83, 024014 – Published 12 January, 2011

DOI: https://doi.org/10.1103/PhysRevD.83.024014

Abstract

We calculate stellar oscillations, including the hadron-quark mixed phase, considering finite-size effects. We find that it is possible to distinguish whether the density discontinuity exists or not in the stars, even if one observes the gravitational waves of the fundamental mode. Additionally, the normalized eigenfrequencies of pressure modes depend strongly on the stellar mass and on the adopted equation of state. In particular, in spite of the fact that the radius of the neutron star with 1.4M⊙, which is the standard mass, is almost independent of the equation of state with quark matter, the frequencies of the pressure modes depend on the adopted equation of state. Thus, via observing the many kinds of gravitational waves, it will be possible to make a restriction on the equation of state.

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Phys. Rev. D 83, 024014– Published 12 January, 2011
  • Received 28 October 2010

© 2011 The American Physical Society

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