### Abstract

Context. Solutions of the magnetohydrostatic (MHS) equations are very important for modelling astrophysical plasmas, such as the coronae of magnetized stars. Realistic models should be three-dimensional, i.e., should not have any spatial symmetries, but finding three-dimensional solutions of the MHS equations is a formidable task. Aims. We present a general theoretical framework for calculating three-dimensional MHS solutions outside massive rigidly rotating central bodies, together with example solutions. A possible future application is to model the closed field region of the coronae of fast-rotating stars. Methods. As a first step, we present in this paper the theory and solutions for the case of a massive rigidly rotating magnetized cylinder, but the theory can easily be extended to other geometries, We assume that the solutions are stationary in the co-rotating frame of reference. To simplify the MHS equations, we use a special form for the current density, which leads to a single linear partial differential equation for a pseudo-potential U. The magnetic field can be derived from U by differentiation. The plasma density, pressure, and temperature are also part of the solution. Results. We derive the fundamental equation for the pseudo-potential both in coordinate independent form and in cylindrical coordinates. We present numerical example solutions for the case of cylindrical coordinates.

Original language | English |
---|---|

Article number | A38 |

Journal | Astronomy and Astrophysics |

Volume | 514 |

Issue number | 3 |

DOIs | |

Publication status | Published - May 7 2010 |

### Fingerprint

### Keywords

- Magnetic fields
- Magnetohydrodynamics (MHD)
- Stars: activity
- Stars: coronae
- Stars: magnetic field

### ASJC Scopus subject areas

- Astronomy and Astrophysics
- Space and Planetary Science

### Cite this

*Astronomy and Astrophysics*,

*514*(3), [A38]. https://doi.org/10.1051/0004-6361/200913723

**Three-dimensional solutions of the magnetohydrostatic equations : Rigidly rotating magnetized coronae in cylindrical geometry.** / Al-Salti, N.; Neukirch, T.; Ryan, R.

Research output: Contribution to journal › Article

*Astronomy and Astrophysics*, vol. 514, no. 3, A38. https://doi.org/10.1051/0004-6361/200913723

}

TY - JOUR

T1 - Three-dimensional solutions of the magnetohydrostatic equations

T2 - Rigidly rotating magnetized coronae in cylindrical geometry

AU - Al-Salti, N.

AU - Neukirch, T.

AU - Ryan, R.

PY - 2010/5/7

Y1 - 2010/5/7

N2 - Context. Solutions of the magnetohydrostatic (MHS) equations are very important for modelling astrophysical plasmas, such as the coronae of magnetized stars. Realistic models should be three-dimensional, i.e., should not have any spatial symmetries, but finding three-dimensional solutions of the MHS equations is a formidable task. Aims. We present a general theoretical framework for calculating three-dimensional MHS solutions outside massive rigidly rotating central bodies, together with example solutions. A possible future application is to model the closed field region of the coronae of fast-rotating stars. Methods. As a first step, we present in this paper the theory and solutions for the case of a massive rigidly rotating magnetized cylinder, but the theory can easily be extended to other geometries, We assume that the solutions are stationary in the co-rotating frame of reference. To simplify the MHS equations, we use a special form for the current density, which leads to a single linear partial differential equation for a pseudo-potential U. The magnetic field can be derived from U by differentiation. The plasma density, pressure, and temperature are also part of the solution. Results. We derive the fundamental equation for the pseudo-potential both in coordinate independent form and in cylindrical coordinates. We present numerical example solutions for the case of cylindrical coordinates.

AB - Context. Solutions of the magnetohydrostatic (MHS) equations are very important for modelling astrophysical plasmas, such as the coronae of magnetized stars. Realistic models should be three-dimensional, i.e., should not have any spatial symmetries, but finding three-dimensional solutions of the MHS equations is a formidable task. Aims. We present a general theoretical framework for calculating three-dimensional MHS solutions outside massive rigidly rotating central bodies, together with example solutions. A possible future application is to model the closed field region of the coronae of fast-rotating stars. Methods. As a first step, we present in this paper the theory and solutions for the case of a massive rigidly rotating magnetized cylinder, but the theory can easily be extended to other geometries, We assume that the solutions are stationary in the co-rotating frame of reference. To simplify the MHS equations, we use a special form for the current density, which leads to a single linear partial differential equation for a pseudo-potential U. The magnetic field can be derived from U by differentiation. The plasma density, pressure, and temperature are also part of the solution. Results. We derive the fundamental equation for the pseudo-potential both in coordinate independent form and in cylindrical coordinates. We present numerical example solutions for the case of cylindrical coordinates.

KW - Magnetic fields

KW - Magnetohydrodynamics (MHD)

KW - Stars: activity

KW - Stars: coronae

KW - Stars: magnetic field

UR - http://www.scopus.com/inward/record.url?scp=77952038903&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=77952038903&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/200913723

DO - 10.1051/0004-6361/200913723

M3 - Article

VL - 514

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 3

M1 - A38

ER -