Magnetohydrodynamic (MHD) simulation of solar prominence formation

Thesis/Dissertation · Thu Jan 01 04:00:00 EST 1987

OSTI ID:6997950

Bao, J

Formation of Kippenhahn-Schluter type solar prominences by chromospheric mass injection is studied via numerical simulation. The numerical model is based on a two-dimensional, time-dependent magnetohydrodynamic (MHD) theory. In addition, an analysis of gravitational thermal MHD instabilities related to condensation is performed by using the small-perturbation method. The conclusions are: (1) Both quiescent and active-region prominences can be formed by chromospheric mass injection, provided certain optimum conditions are satisfied. (2) Quiescent prominences cannot be formed without condensation, though enough mass is supplied from chromosphere. The mass of a quiescent prominence is composed of both the mass injected from the chromosphere and the mass condensed from the corona. On the other hand, condensation is not important to active region prominence formation. (3) In addition to channeling and supporting effects, the magnetic field plays another important role, i.e. containing the prominence material. (4) In the model cases, prominences are supported by the Lorentz force, the gas-pressure gradient and the mass-injection momentum. (5) Due to gravity, more MHD condensation instability modes appear in addition to the basic condensation mode.

• Research Organization: Alabama Univ., Huntsville (USA)
• OSTI ID: 6997950
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
640430 -- Fluid Physics-- Magnetohydrodynamics
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
75 CONDENSED MATTER PHYSICS
SUPERCONDUCTIVITY AND SUPERFLUIDITY
ATMOSPHERES
CHROMOSPHERE
FLUID MECHANICS
HYDRODYNAMICS
LORENTZ FORCE
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MASS TRANSFER
MECHANICS
PRODUCTION
SIMULATION
SOLAR ACTIVITY
SOLAR ATMOSPHERE
SOLAR PROMINENCES
VAPOR CONDENSATION