A new class of g-modes in neutron stars
نویسندگان
چکیده
منابع مشابه
A NEW CLASS OF g-MODES IN NEUTRON STARS
Beca~se. a n~utron star is ~orn hot, its internal composition is close to chemical equilibrium. In the fluid core, thts tmphes_ that _the rat!o of the_ number densities of charged particles (protons and electrons) to neutrons, x ~.ncfnn, ts an mcreasmg function of the mass density. This composition gradient stably stratifies the m~tter glVlng ~ise to a Br~nt-Viiisiilii frequency N ~ (xgj2H) 112...
متن کاملSecular Instability of g-Modes in Rotating Neutron Stars
Gravitational radiation tends to drive gravity modes in rotating neutron stars unstable. For an inviscid star, the instability sets in when the rotation frequency is about 0.7 times the corresponding mode frequency of the nonrotating star. Neutron stars with spin frequencies > ∼ 100 Hz are susceptible to this instability, with growth time of order years. However, it is likely that viscous dissi...
متن کاملThermal g-modes and unexpected convection in superfluid neutron stars
We suggest that specific thermal low-frequency g-modes can exist in superfluid neutron stars. They can be excited in the matter with a nonzero gradient of entropy per electron. We determine the Brunt-Väisälä frequency for these modes and demonstrate that they can be unstable with respect to convection. The criterion for the instability onset (analogue of the well-known Schwarzschild criterion) ...
متن کاملRelativistic g-modes in rapidly rotating neutron stars
We study the g-modes of fast rotating neutron in the general relativistic Cowling approximation. Our background models take into account the buoyant force due to composition gradients. We compare the Newtonian results of Passamonti et al. (2009) with our relativistic ones and we find an excellent qualitative agreement.
متن کاملA new class of unstable modes of rotating relativistic stars
The first numerical study of axial (toroidal) pulsation modes of a slowly rotating relativistic star is presented. The calculation includes terms of first order in ǫ ≡ Ω √ R3/M << 1 (R is the radius, M is the mass and Ω is the rotation frequency of the star), and accounts for effects due to the coriolis force. Effects due to the centrifugal flattening of the star enter at order ǫ and are not in...
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: The Astrophysical Journal
سال: 1992
ISSN: 0004-637X,1538-4357
DOI: 10.1086/171645