The theory of ideal magnetohydrodynamic turbulence in cylindrical geometry is used to study the steady-state structure of a coronal loop. The pressure profile is derived from MHD equations by representing the velocity and magnetic fields as the superposition of Chandrasekhar-Kendall functions. Such
Temporal behaviour of pressure in solar coronal loops
โ Scribed by K. Sasidharan; T. D. Sreedharan; R. Pratap; V. Krishan
- Publisher
- Springer
- Year
- 1995
- Tongue
- English
- Weight
- 628 KB
- Volume
- 157
- Category
- Article
- ISSN
- 0038-0938
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