28,637 research outputs found
Discriminating hadronic and quark stars through gravitational waves of fluid pulsation modes
We investigate non-radial oscillations of hadronic, hybrid and pure
self-bound strange quark stars with maximum masses above the mass of the
recently observed massive pulsars PSR J1614-2230 and PSR J0348-0432 with . For the hadronic equation of state we employ different
parametrizations of a relativistic mean-field model and for quark matter we use
the MIT bag model including the effect of strong interactions and color
superconductivity. We find that the first pressure mode for strange quark stars
has a very different shape than for hadronic and hybrid stars. For strange
quarks stars the frequency of the p1 mode is larger than 6 kHz and diverge at
small stellar masses, but for hadronic and hybrid stars it is in the range 4-6
kHz. This allows an observational identification of strange stars even if extra
information such as the mass, the radius or the gravitational redshift of the
object is unavailable or uncertain. Also, we find as in previous works that the
frequency of the g-mode associated with the quark-hadron discontinuity in a
hybrid star is in the range 0.4-1 kHz for all masses. Thus, compact objects
emitting gravitational waves above 6 kHz should be interpreted as strange quark
stars and those emitting a signal within 0.4-1 kHz should be interpreted as
hybrid stars.Comment: 7 pages, 5 figure
- β¦