SIMULATION OF MAGNETOHYDRODYNAMIC SHOCK WAVE GENERATION, PROPAGATION, AND HEATING IN THE PHOTOSPHERE AND CHROMOSPHERE USING A COMPLETE ELECTRICAL CONDUCTIVITY TENSOR
- Advanced Technologies Group, West Virginia High Technology Consortium Foundation, 1000 Galliher Drive, Fairmont, WV 26554 (United States)
An electrical conductivity tensor is used in a 1.5D magnetohydrodynamic (MHD) simulation to describe how MHD shock waves may form, propagate, and heat the photosphere and chromosphere by compression and resistive dissipation. The spatial resolution is 1 km. A train of six shock waves is generated by a sinusoidal magnetic field driver in the photosphere with a period T = 30 s, mean of 500 G, and variation of 250 G. The duration of the simulation is 200 s. Waves generated in the photosphere evolve into shock waves at a height z approx 375 km above the photosphere. The transition of the atmosphere from weakly to strongly magnetized with increasing height causes the Pedersen resistivity eta{sub P} to increase to approx2000 times the Spitzer resistivity. This transition occurs over a height range of a few hundred kilometers near the temperature minimum of the initial state at z approx 500 km. The initial state is a model atmosphere derived by Fontenla et al., plus a background magnetic field. The increase in eta{sub P} is associated with an increase in the resistive heating rate Q. Shock layer thicknesses are approx10-20 km. They are nonzero due to the presence of resistive dissipation, so magnetization-induced resistivity plays a role in determining shock structure, and hence the compressive heating rate Q{sub c} . At t = 200 s the solution has the following properties. Within shock layers, Q{sub maximum} approx 1.4-7 erg cm{sup -3} s{sup -1}, and Q{sub c,maximum} approx 10-10{sup 3} Q{sub maximum}. Between shock waves, and at some points within shock layers, Q{sub c} < 0, indicating cooling by rarefaction. The integrals of Q and Q{sub c} over the shock wave train are F approx 4.6 x 10{sup 6} erg cm{sup -2} s{sup -1} and F{sub c} approx 1.24 x 10{sup 9} erg cm{sup -2} s{sup -1}. A method based on the thermal, mechanical, and electromagnetic energy conservation equations is presented for checking the accuracy of the numerical solution, and gaining insight into energy flow and transformation. The method can be applied to higher dimensional simulations. It is suggested that observations be performed to map out the transition region across which the transition from weakly ionized, weakly magnetized plasma to weakly ionized, strongly magnetized plasma occurs, and to correlate it with net radiative loss.
- OSTI ID:
- 21392484
- Journal Information:
- Astrophysical Journal, Vol. 708, Issue 1; Other Information: DOI: 10.1088/0004-637X/708/1/268; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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COSMOLOGY AND ASTRONOMY
CHROMOSPHERE
COMPRESSION
ELECTRIC CONDUCTIVITY
ENERGY CONSERVATION
HEATING
HEATING RATE
INTEGRALS
MAGNETIC FIELDS
MAGNETIZATION
MAGNETOHYDRODYNAMICS
NUMERICAL SOLUTION
PHOTOSPHERE
PLASMA
S WAVES
SHOCK WAVES
SIMULATION
SPATIAL RESOLUTION
SUN
TENSORS
THICKNESS
ATMOSPHERES
DIMENSIONS
ELECTRICAL PROPERTIES
FLUID MECHANICS
HYDRODYNAMICS
MAIN SEQUENCE STARS
MATHEMATICAL SOLUTIONS
MECHANICS
PARTIAL WAVES
PHYSICAL PROPERTIES
RESOLUTION
SOLAR ATMOSPHERE
STARS
STELLAR ATMOSPHERES