Mechanism of r-mode stability in young rapidly rotating pulsars

Abstract

We demonstrate that stability of r-modes in young rapidly rotating pulsars might be explained if one takes into account strong medium modifications of the nucleon-nucleon interaction because of the softening of pionic degrees of freedom in dense nucleon matter. Presence of the efficient direct Urca processes is not required. Within our model the most rapidly rotating observed young pulsar PSR J0537-6910 should have the mass $\ge 1.8M_{\odot }$.

arXiv comment4 pages, 3 figures, minor corrections, to be published in Eur. Phys. J. A

References in corpus (20)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• The equation of state for nucleon matter and neutron star structure
• A new class of unstable modes of rotating relativistic stars
• Gravitational Radiation Instability in Hot Young Neutron Stars
• Axial instability of rotating relativistic stars
• The Cooling of Compact Stars
• The r-mode instability in rotating neutron stars
• Analytical representations of unified equations of state of neutron-star matter
• Polarization contributions to the spin-dependence of the effective interaction in neutron matter
• Cooling of Neutron Stars. Hadronic Model
• Shear viscosity in neutron star cores
• Bulk viscosity in superfluid neutron star cores. II. Modified Urca processes in $npe\mu$ matter
• On the Cooling of the Neutron Star in Cassiopeia A
• Gravitational wave emission and spindown of young pulsars
• Nuclear medium cooling scenario in the light of new Cas A cooling data and the 2 M_sun pulsar mass measurements
• Medium Effects in Cooling of Neutron Stars and $3P_2$ Neutron Gap
• The Spin Period, Luminosity and Age Distributions of Anomalous X-Ray Pulsars
• The role of $r$-mode damping in the thermal evolution of neutron stars
• Radiative viscosity of neutron stars

Cited by in corpus (4)

• Viscosity of neutron star matter and $r$-modes in rotating pulsars
• Cooling of neutron stars in "nuclear medium cooling scenario" with stiff equation of state including hyperons
• Structure formation during phase transitions in strongly interacting matter
• Influence of the nuclear matter equation of state on the r-mode instability using the finite-range simple effective interaction