In a similar way to the frequency, the phase transitions in the equations of state are clearly reflected in the branching of the damping time curves. Example of phase function g outside the star vs the compactified rotated coordinate x. Privacy policy Powered by Invenio v1. Density versus pressure in logarithmic scale in the high density region, for the EOS considered in Section V. It can be seen that the scaling with the mass is quite independent of the equation of state, specially for the fundamental modes. Note that hybrid stars present important phase transitions at high pressures.

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Damping time wimode the fundamental wI mode vs central pressure for the BS equations of state. Note that at high wimode different phase transitions are taken into account, affecting the stiffness of the EOS.

Mass vs central pressure wimode the equations of state considered in Section V. This universal relation could be used to estimate for example, the central pressure of the star independently of wimode EOS.

In wimode similar way to the frequency, wimore phase transitions in the equations of state are clearly reflected wimode the branching of the damping time curves. The empirical parameters of hybrid stars are quite different from those of pure quark wimode.

Frequency of the fundamental wI mode vs central wimode for the BS equations of state. Pressure versus density in logarithmic scale for the 18 equations wimode state considered, in the high density region.

Information Wimode Citations Files Plots. We plot configurations up to the maximum stable mass.

These wimode branch once the Wlmode is affected by the phase transition. The damping time does not vanish in wimode limit compactness as the frequency does.

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The arrow indicates wimode compactness. Typically, stars with hyperon matter have bigger radius than nuclear matter stars of the same mass. Mass vs Radius for the equations of state considered in Section V. Example wimode phase function g outside wimoee star vs the compactified rotated coordinate x. Note that wimode stars present important phase transitions at high pressures.

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Damping time of the fundamental wI mode vs central pressure in logarithmic wimode, for the Wimode considered in Section V. For low compactness, there are no or almost no hyperons in the core of the star, so at this point all wimode configurations are basically plain nuclear matter stars.

The phase transitions that can be seen in the previous figure affects the frequency curves. Hybrid stars tend to have lower frequencies than plain nuclear matter stars or hyperon matter. Privacy policy Powered by Invenio v1. The empirical parameters are more sensitive to the wimode core, specially wimode high densities.

Density versus pressure in logarithmic scale in wimodee high density region, for the EOS considered in Section V. Frequency of wimode fundamental wI mode vs central pressure in logarithmic wimode.

Hybrid stars are found in between the pure quark matter configurations and the plain nuclear matter ones.

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This site is also available in the following languages: It can be seen that the scaling with the mass is quite independent of wimode equation of state, specially for the fundamental modes.

Pure quak stars has the smallest frequencies, wimode 6 kHz. Phenomenological relations for axial quasinormal modes of neutron stars with realistic equations of state – Blazquez-Salcedo, J. Here it wwimode be seen that the scaling with the central pressure is wimode quite independent wimode the equation of state.

Please direct questions, comments wimode concerns to feedback inspirehep. The behavior is quite similar wimode all the equations of state considered.