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Non-linear Convection with Variable Viscosity and Thermal Conductivity

Published online by Cambridge University Press:  25 April 2016

R. van der Borght  and
B. E. Waters
R. van der Borght
Affiliation:
Department of Mathematics, Monash University, Melbourne
B. E. Waters
Affiliation:
Department of Mathematics, Monash University, Melbourne
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Extract

In his studies of the temperature fluctuation in the solar photosphere P. R. Wilson came to the conclusion that, in order to explain Edmond’s r.m.s. intensity fluctuation distribution against heliocentric angle, one is led, using two dimensional solutions for the equation of radiative transfer, to the existence of a sharp temperature fluctuation of about 660 K r.m.s. at a depth of 250 km below τ5000 = 0.03 and that this temperature fluctuation decreases sharply in the next 70 km. There also seems to be an indication that there exists a second temperature fluctuation maximum at a depth of approximately 100 km below the first one.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 1 , July 1971 , pp. 47 - 48
Copyright
Copyright © Astronomical Society of Australia 1971

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References

1 Wilson, P. R., Solar Physics, 6, 364 (1969).CrossRefGoogle Scholar
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