MG15 - Talk detail

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Abstract

We study radial oscillations of hybrid non-rotating neutron stars composed by a quark matter core and hadronic external layers. We compute the oscillation spectrum focusing on the effects of slow and rapid phase transitions at the quark-hadron interface. We show that the usual static stability condition ∂M/∂ρc ≥ 0, where ρc is the central density of a star whose total mass is M, remains always true for rapid transitions but breaks down in general for slow transitions. In fact, for slow transitions we find that the frequency of the fundamental mode can be a real number (indicating stability) even for some branches of stellar models that verify ∂M/∂ρc ≤ 0. Thus, when secular instabilities are suppressed, as expected below some critical stellar rotation rate, it would be possible the existence of twin, triplet or even multiplet stars with the same gravitational mass but different radii, with one or more of the counterparts having ∂M/∂ρc ≤ 0. We explore some astrophysical consequences of these results.

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