Anisotropic convection in rotating proto-neutron stars

Abstract

We study the conditions for convective instability in rotating, non-magnetic proto--neutron stars. The criteria that determine stability of nascent neutron stars are analogous to the Solberg--Hoiland conditions but including the presence of lepton gradients. Our results show that, for standard angular velocity profiles, convectively unstable modes with wave-vectors parallel to the rotation axis are suppressed by a stable angular momentum profile, while unstable modes with wave-vectors perpendicular to the axis remain unaltered. Since the wave-vector is perpendicular to the velocity perturbation, the directional selection of the unstable modes may result in fluid motions along the direction of the rotation axis. This occurs in rigidly rotating stars as well as in the inner core of differentially rotating stars. Our results provide a natural source of asymmetry for proto--neutron stars with the only requirement that angular velocities be of the order of the convective characteristic frequency.

arXiv comment5 pages, 4 figures, final version to appear in A&A

References in corpus (12)

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Cited by in corpus (12)

• A New Mechanism for Core-Collapse Supernova Explosions
• Explosion Mechanism, Neutrino Burst, and Gravitational Wave in Core-Collapse Supernovae
• Rotating Stars in Relativity
• Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions
• Long gravitational-wave transients and associated detection strategies for a network of terrestrial interferometers
• General relativistic simulations of pasive-magneto-rotational core collapse with microphysics
• The Effect of Neutrino Radiation on Magnetorotational Instability in Proto-Neutron Stars
• Nonaxisymmetric Magnetorotational Instability in Proto-Neutron Stars
• Contraction of cold neutron star due to in the presence a quark core
• Identification of noise artifacts in searches for long-duration gravitational-wave transients
• Mixing zones in magnetized differentially rotating stars
• Neutrino transport and hydrodynamic stability of rotating proto-neutron stars