Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.0409s&link_type=abstract
American Astronomical Society Meeting 208, #4.09; Bulletin of the American Astronomical Society, Vol. 38, p.82
Astronomy and Astrophysics
Astronomy
Scientific paper
We study the role of spin-down of isolated neutron stars in driving quark deconfinement in their high density core. Assuming spin-down to be solely due to magnetic braking, we obtain typical timescales to quark deconfinement for neutron stars that are born with Keplerian frequencies. Employing different equations of state (EOS), we determine the minimum and maximum neutron star masses that will allow for deconfinement via spin-down only. We find that the time to reach deconfinement is strongly dependent on the magnetic field and that this time is least for EOS that support the largest minimum mass at zero spin, unless rotational effects on stellar structure are large. For a fiducial critical density of five times nuclear saturation density for the transition to the quark phase, we find that neutron stars lighter than 1.5 solar masses cannot reach a deconfined phase. Depending on the EOS, neutron stars of more than 1.5 solar masses can enter a quark phase only if they are spinning faster than about 3 milliseconds as observed now, whereas larger spin periods imply that they are either already quark stars or will never become one.
Jaikumar Prashanth
Ouyed Rachid
Staff Jan E.
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