Published 1988
| Version v1
Book
Dynamics of magnetic and velocity fields in coronal loops
Creators
Description
The coronal loop plasma is represented by a superposition of the three lowest order Chandrasekhar-Kendall modes. The temporal evolution of the velocity and magnetic field in each of these modes is determined using ideal MHD equations under two simplified cases, viz (1) allowing small departures from the equilibrium and (2) the pump approximation. 5 references
Additional details
Publishing Information
- Publisher
- National Solar Observatory.
- Imprint Place
- Sunspot, NM (USA)
- Imprint Title
- Solar and stellar coronal structure and dynamics; Proceedings of the Ninth Sacramento Peak Summer Symposium, Sunspot, NM, Aug. 17-21, 1987
- Journal Page Range
- p. 236-247.
Conference
- Title
- solar and stellar coronal structure and dynamics.
- Acronym
- 9. Sacramento peak summer symposium
- Dates
- 17-21 Aug 1987.
- Place
- Sunspot, NM (USA).
INIS
- Country of Publication
- United States
- Country of Input or Organization
- United States
- INIS RN
- 20039109
- Subject category
- S79: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;
- Resource subtype / Literary indicator
- Conference
- Descriptors DEI
- DYNAMICS; HYDROMAGNETIC WAVES; MAGNETIC FIELDS; PLASMA; SOLAR CORONA; SOLAR WIND; VELOCITY
- Descriptors DEC
- ATMOSPHERES; MECHANICS; SOLAR ACTIVITY; SOLAR ATMOSPHERE; STELLAR ACTIVITY; STELLAR ATMOSPHERES; STELLAR CORONAE; STELLAR WINDS