Axisymmetric plasma equilibrium in gravitational and magnetic fields

Krasheninnikov, S. I.; Catto, Peter J.

doi:10.1134/s1063780x15120065

Cited by 1 publication

(2 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We have used the procedure of Krasheninnikov et al. (1999, 2000), Catto & Krasheninnikov (2015), Krasheninnikov & Catto (2015) to generalize the separable form of the Grad–Shafranov equation derived there to include a toroidal magnetic field. For the lower cases considered in § 5, the new feature considered here is the need to retain a toroidal magnetic field.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…We desire the solution to be up–down symmetric having the normalization , satisfying the boundary condition and having no zero crossings for . Solutions with zero crossings exist, but poloidal magnetic field reversal is considered in a separate investigation (Krasheninnikov & Catto 2015). Moreover, up–down asymmetric solutions are possible, but will not be considered herein.…”

Section: Separable Formmentioning

confidence: 99%

See 1 more Smart Citation

Axisymmetric global gravitational equilibrium for magnetized, rotating hot plasma

2015

View full text Add to dashboard Cite

We present analytic solutions for three-dimensional magnetized axisymmetric equilibria confining rotating hot plasma in a gravitational field. Our up–down symmetric solution to the full Grad–Shafranov equation can exhibit equatorial plane localization of the plasma density and current, resulting in disk equilibria for the plasma density. For very weak magnetic fields and high plasma pressure, we find strongly rotating thin plasma disk gravitational equilibria that satisfy strict Keplerian motion provided the gravitational energy is much larger than the plasma pressure, which must be large compared to the magnetic energy of the poloidal magnetic field. When the rotational energy exceeds the gravitational energy and it is larger than the plasma pressure, diffuse disk equilibrium solutions continue to exist provided the poloidal magnetic energy remains small. For stronger magnetic fields and lower plasma pressure and rotation, we can also find gravitational equilibria with strong localization to the equatorial plane. However, a toroidal magnetic field is almost always necessary to numerically verify these equilibria are valid solutions in the presence of gravity for the cases considered in Catto & Krasheninnikov (J. Plasma Phys., vol. 81, 2015, 105810301). In all cases both analytic and numerical results are presented.

show abstract