g-mode Oscillations in Hybrid Stars: A Tale of Two Sounds. (arXiv:2101.06349v3 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Jaikumar_P/0/1/0/all/0/1">Prashanth Jaikumar</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Semposki_A/0/1/0/all/0/1">Alexandra Semposki</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Prakash_M/0/1/0/all/0/1">Madappa Prakash</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Constantinou_C/0/1/0/all/0/1">Constantinos Constantinou</a>
We study the principal core g-mode oscillation in hybrid stars containing
quark matter and find that they have an unusually large frequency range
($approx$ 200 – 600 Hz) compared to ordinary neutron stars or self-bound quark
stars of the same mass. Theoretical arguments and numerical calculations that
trace this effect to the difference in the behaviour of the equilibrium and
adiabatic sound speeds in the mixed phase of quarks and nucleons are provided.
We propose that the sensitivity of core g-mode oscillations to non-nucleonic
matter in neutron stars could be due to the presence of a mixed quark-nucleon
phase. Based on our analysis, we conclude that for binary mergers where one or
both components may be a hybrid star, the fraction of tidal energy pumped into
resonant g-modes in hybrid stars can exceed that of a normal neutron star by a
factor of 2-3, although resonance occurs during the last stages of inspiral. A
self-bound star, on the other hand, has a much weaker tidal overlap with the
g-mode. The cumulative tidal phase error in hybrid stars, $Deltaphicong$ 0.5
rad, is comparable to that from tides in ordinary neutron stars, presenting a
challenge in distinguishing between the two cases. However, should the
principal g-mode be excited to sufficient amplitude for detection in a
post-merger remnant with quark matter in its interior, its frequency would be a
possible indication for the existence of non-nucleonic matter in neutron stars.
We study the principal core g-mode oscillation in hybrid stars containing
quark matter and find that they have an unusually large frequency range
($approx$ 200 – 600 Hz) compared to ordinary neutron stars or self-bound quark
stars of the same mass. Theoretical arguments and numerical calculations that
trace this effect to the difference in the behaviour of the equilibrium and
adiabatic sound speeds in the mixed phase of quarks and nucleons are provided.
We propose that the sensitivity of core g-mode oscillations to non-nucleonic
matter in neutron stars could be due to the presence of a mixed quark-nucleon
phase. Based on our analysis, we conclude that for binary mergers where one or
both components may be a hybrid star, the fraction of tidal energy pumped into
resonant g-modes in hybrid stars can exceed that of a normal neutron star by a
factor of 2-3, although resonance occurs during the last stages of inspiral. A
self-bound star, on the other hand, has a much weaker tidal overlap with the
g-mode. The cumulative tidal phase error in hybrid stars, $Deltaphicong$ 0.5
rad, is comparable to that from tides in ordinary neutron stars, presenting a
challenge in distinguishing between the two cases. However, should the
principal g-mode be excited to sufficient amplitude for detection in a
post-merger remnant with quark matter in its interior, its frequency would be a
possible indication for the existence of non-nucleonic matter in neutron stars.
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