Publication

Calculation of global modes via ballooning formalisms

Wilfred Anthony Cooper
1997
Journal Articles

Abstract

Ballooning theory is an asymptotic method for treating modes with short wavelength across the magnetic field lines but essentially no phase variation along the lines. The latter constraint leads to problems with maintaining the physically required poloidal and toroidal periodicity, which can be solved in various ways. In this paper we review the approach of Dewar and Glasser, which applies to general three-dimensional equilibria, and also review some recent applications of the formalism to a heliotron/torsatron test case.

Official source

https://infoscience.epfl.ch/entities/publication/93d3e1dc-f6e5-42dd-9b1f-b8c2f944758b

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Wilfred Anthony Cooper
1997
Journal Articles

Abstract

Official source

https://infoscience.epfl.ch/entities/publication/93d3e1dc-f6e5-42dd-9b1f-b8c2f944758b

About this result

Related concepts (29)

Magnetic field

A magnetic field is a vector field that describes the magnetic influence on moving electric charges, electric currents, and magnetic materials. A moving charge in a magnetic field experiences a force perpendicular to its own velocity and to the magnetic field. A permanent magnet's magnetic field pulls on ferromagnetic materials such as iron, and attracts or repels other magnets.

Earth's magnetic field

Earth's magnetic field, also known as the geomagnetic field, is the magnetic field that extends from Earth's interior out into space, where it interacts with the solar wind, a stream of charged particles emanating from the Sun. The magnetic field is generated by electric currents due to the motion of convection currents of a mixture of molten iron and nickel in Earth's outer core: these convection currents are caused by heat escaping from the core, a natural process called a geodynamo.

Interplanetary magnetic field

The interplanetary magnetic field (IMF), now more commonly referred to as the heliospheric magnetic field (HMF), is the component of the solar magnetic field that is dragged out from the solar corona by the solar wind flow to fill the Solar System. The coronal and solar wind plasmas are highly electrically conductive, meaning the magnetic field lines and the plasma flows are effectively "frozen" together and the magnetic field cannot diffuse through the plasma on time scales of interest.

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Calculation of global modes via ballooning formalisms

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