منابع مشابه
Studying Ism Magnetic Fields and Turbulent Regimes from Polarimetric Maps
Polarimetric maps have been used for the characterization of the magnetic field in molecular clouds. However, it is difficult to determine the 3-dimensional properties of these regions from the projected maps. For that reason, numerical simulations can be used as benchmarks for polarimetric measurements, and eventually reveal more about the interplay of turbulence and the magnetic field lines. ...
متن کاملMagnetic Fields Ignorable Magnetic Fields Non Ignorable Magnetic Fields Important Magnetic Fields Dominant
Magnetic fields are considered to be dominant when εB ≥ εK , being εB = B /8π the magnetic energy density and εK = 1/2ρθ 2 the rotation energy density, for a conventional moderate B= 1 μG. They are considered to be negligible when εB < εK for B ∼ 10μG. With no assumption and no theoretical calculation, we show that magnetic fields cannot be ignored in the outer parts of a galaxy like the Milky ...
متن کاملCan we ignore magnetic fields in studies of PN formation, shaping and interaction with the ISM?
In a quest for better understanding the shaping mechanism of planetary nebulae (PNs) I published many papers in the past (e.g., Soker 2004a) all of which came to the same conclusion: For the formation of non-spherical PNs a companion is required, wether stellar or substellar. This results from the basic assumption that angular momentum is a conserved physics quantity. As trivial as this may sou...
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 کاملNon-dipolar magnetic fields in Ap stars
An arbitrary initial magnetic field in an A star evolves into a stable equilibrium. Simulations are presented of the formation of non-axisymmetric equilibria consisting of twisted flux tubes meandering under the surface of the star, and analytic arguments are given relating the stability and form of these equilibria. These results may help to explain observations of Ap stars with very non-dipol...
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2007
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921307012550