Published October 1976
| Version v1
Report
Dynamics of the density inversion zone of a one solar mass star
Creators
Description
The density inversion zone of a one solar mass star was studied by two dimensional numerical fluid dynamics calculations. The turbulent convection in this unstable layer provides a larger turbulent heat flux than predicted by the mixing length theory, thereby removing the density inversion found in the equilibrium model. The instability also causes a periodic sequence of buoyantly rising bubbles that have all of the characteristics of the solar granulation. 10 figs
Additional details
Publishing Information
- Imprint Title
- Proceedings of the solar and stellar pulsation conference
- Imprint Pagination
- p. 36-46.
- Report number
- LA--6544-C
Conference
- Title
- Solar and stellar pulsation conference.
- Dates
- 2 Aug 1976.
- Place
- Los Alamos, New Mexico, United States of America (USA).
INIS
- Country of Publication
- United States
- Country of Input or Organization
- United States
- INIS RN
- 8316847
- Subject category
- S79: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;
- Resource subtype / Literary indicator
- Conference
- Descriptors DEI
- BUBBLES; CONVECTION; HYDROSTATICS; SOLAR GRANULATION; STAR MODELS; SUN; TURBULENCE
- Descriptors DEC
- ENERGY TRANSFER; HEAT TRANSFER; MATHEMATICAL MODELS; SOLAR ACTIVITY; STARS