Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974impm.nasa..203y&link_type=abstract
"In its Interplanet. Medium and Phys. of the Magnetosphere (NASA-TT-F-784) p 203-223 (SEE N75-13707 04-90) Transl. into ENGLIS
Astronomy and Astrophysics
Astronomy
Convective Flow, Plasma Turbulence, Stellar Envelopes, Thermal Instability, Astronomical Models, Chromosphere, Main Sequence Stars, Plasma-Electromagnetic Interaction, Stellar Rotation
Scientific paper
The nonstationary convection that arises due to thermal instability in the envelopes of lower Main Sequence stars (and the sun in particular) is investigated. The convection that arises in the envelopes as a result of thermal instability is of nonstationary turbulent nature. It is shown that construction of a consistent model of the zones of turbulent convection in the stars requires the use of the complete heat flux equation with consideration of the terms that appear because of turbulence. Expressions for these additional terms in terms of averaged characteristics of the motion and eddy viscosity coefficients are derived on the basis of the Prandtl-Wasiutinsky theory.
No associations
LandOfFree
Thermal instability and energy relations in the convective envelopes of slowly rotating stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Thermal instability and energy relations in the convective envelopes of slowly rotating stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Thermal instability and energy relations in the convective envelopes of slowly rotating stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1764097