Anisotropic convection in rotating proto-neutron stars
نویسندگان
چکیده
منابع مشابه
Anisotropic convection in rotating proto-neutron stars
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–Høiland 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 a...
متن کاملGravitational Waves from Rotating Proto-Neutron Stars
We study the effects of rotation on the quasi normal modes (QNMs) of a newly born proto neutron star (PNS) at different evolutionary stages, until it becomes a cold neutron star (NS). We use the Cowling approximation, neglecting spacetime perturbations, and consider different models of evolving PNS. The frequencies of the modes of a PNS are considerably lower than those of a cold NS, and are fu...
متن کاملNeutrino transport and hydrodynamic stability of rotating proto-neutron stars
Aims. We study stability of differentially rotating non-magnetic proto-neutron stars. Methods. Linear stability properties are considered taking into account neutrino transport. Results. If neutrino transport is efficient, the star can be subject to a diffusive instability that can occur even in the convectively stable region. The instability arises on the time-scale comparable to the time-scal...
متن کاملProto-neutron and Neutron Stars
It has been shown that effective chiral hadronic models can satisfactorily describe nuclear matter, properties of finite nuclei as well as the structure of neutron stars1. While most of the approaches are based on variations of the linear sigma model or its non-linear realization, in the approach discussed here the scalar sigma meson serves to split the nucleon and its chiral partner (particle ...
متن کاملRotating Neutron Stars
Because of the tremendous densities that exist in the cores of neutron stars, a significant fraction of the matter in the cores of such stars is likely to exist in the form of hyperons. Depending on spin frequency, the hyperon content changes dramatically in rotating neutron stars, as discussed in this paper. PACS. 26.60 +c Nuclear matter aspects of neutron stars – 97.60.Gb Pulsars – 97.60.Jd N...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2004
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20035924