Galactic Dynamos Without Sharp Boundaries: Non-Axisymmetric Fields in Axisymmetric Disks?
نویسندگان
چکیده
منابع مشابه
Non-axisymmetric instability of axisymmetric magnetic fields
Context. The MHD instabilities can generate complex field topologies even if the initial field configuration is a very simple one. Aims. We consider the stability properties of magnetic configurations containing a toroidal and an axial field. In this paper, we concentrate mainly on the behavior of non-axisymmetric perturbations in axisymmetric magnetic configurations. Methods. The stability is ...
متن کاملTransport barriers in non-axisymmetric magnetic fields
A transport barrier which is characterized by the steeper temperature or/and density gradient has been observed both in the core region (internal transport barrier : ITB) and edge region (edge transport barrier : ETB) in the plasmas with non-axisymmetric magnetic fields compared with the gyro-Bohm type L-mode transport. A reduction of thermal conductivity and particle diffusivity in these plasm...
متن کاملSharp Hardy-leray Inequality for Axisymmetric Divergence-free Fields
appears for n = 3 in the pioneering Leray’s paper on the Navier-Stokes equations [2]. The constant factor on the right-hand side is sharp. Since one frequently deals with divergence-free fields in hydrodynamics, it is natural to ask whether this restriction can improve the constant in (1.1). We show in the present paper that this is the case indeed if n > 2 and the vector field u is axisymmetri...
متن کاملExact Relativistic Static Charged Dust Disks and Non-axisymmetric Structures
The well-known “displace, cut and reflect” method used to generate disks from given solutions of Einstein field equations is applied to the superposition of two extreme Reissner-Nordström black holes to construct disks made of charged dust and also non-axisymmetric planar distributions of charged dust on the z = 0 plane. They are symmetric with respect to two or one coordinate axes, depending w...
متن کاملAxisymmetric Magnetorotational Instability in Viscous Accretion Disks
Axisymmetric magnetorotational instability (MRI) in viscous accretion disks is investigated by linear analysis and two-dimensional nonlinear simulations. The linear growth of the viscous MRI is characterized by the Reynolds number defined as RMRI ≡ v A/νΩ, where vA is the Alfvén velocity, ν is the kinematic viscosity, and Ω is the angular velocity of the disk. Although the linear growth rate is...
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: Symposium - International Astronomical Union
سال: 1990
ISSN: 0074-1809
DOI: 10.1017/s0074180900189697