Oscillations of superfluid hyperon stars: decoupling scheme and g-modes

Abstract

We analyse the oscillations of general relativistic superfluid hyperon stars, following the approach suggested by Gusakov & Kantor and Gusakov et al. and generalizing it to the nucleon-hyperon matter. We show that the equations governing the oscillations can be split into two weakly coupled systems with the coupling parameters $s_{\rm e}$, $s_{\rm \mu}$, and $s_{\rm str}$. The approximation $s_{\rm e} = s_{\rm \mu} = s_{\rm str} = 0$ (decoupling approximation) allows one to drastically simplify the calculations of stellar oscillation spectra. An efficiency of the presented scheme is illustrated by the calculation of sound speeds in the nucleon-hyperon matter composed of neutrons (n), protons (p), electrons (e), muons ($\mu$), as well as $\rm \Lambda$, ${\rm \Xi}^-$, and ${\rm \Xi}^0$-hyperons. However, the gravity oscillation modes (g-modes) cannot be treated within this approach, and we discuss them separately. For the first time we study the composition g-modes in superfluid hyperon stars with the $\rm npe\mu\Lambda$ core and show that there are two types of g-modes (`muonic' and `$\Lambda$--hyperonic') in such stars. We also calculate the g-mode spectrum and find out that the eigenfrequencies $\nu$ of the superfluid g-modes can be exceptionally large (up to $\nu \approx 742~{\rm Hz}$ for a considered stellar model).