'Mixing length' diaporamas de présentation

EVOLUTION AND INTERNAL STRUCTURE OF RED GIANTS

EVOLUTION AND INTERNAL STRUCTURE OF RED GIANTS. Maurizio Salaris Astrophysics Research Institute Liverpool John Moores University. What stars am I going to talk about?. Kallinger et al. (2010). Adapted from Gallart (1999). From McConnachie et al. (2006). RGB stars as metallicity indicators.

770 views • 65 slides

Weather/Wind Forecasting and Impact of Surface Conditions on Vertical Profile of Horizontal Winds

Weather/Wind Forecasting and Impact of Surface Conditions on Vertical Profile of Horizontal Winds. William A. Gallus, Jr. Dept. of Geological and Atmospheric Sciences June 7, 2012. How might you forecast the weather (or wind in particular)?. Several Methods can be used:.

689 views • 61 slides

Weather/Wind Forecasting and Impact of Surface Conditions on Vertical Profile of Horizontal Winds

Weather/Wind Forecasting and Impact of Surface Conditions on Vertical Profile of Horizontal Winds. William A. Gallus, Jr. Dept. of Geological and Atmospheric Sciences June 7, 2012. How might you forecast the weather (or wind in particular)?. Several Methods can be used:.

687 views • 61 slides

Weather/Wind Forecasting and Impact of Surface Conditions on Vertical Profile of Horizontal Winds

Weather/Wind Forecasting and Impact of Surface Conditions on Vertical Profile of Horizontal Winds. William A. Gallus, Jr. Dept. of Geological and Atmospheric Sciences May 31, 2013. How might you forecast the weather (or wind in particular)?. Several Methods can be used:.

621 views • 61 slides

and now for something completely different...

and now for something completely different. Axion like particles and the transparency of the Universe Malcolm Fairbairn. Based on work with Sergei Troitsky and Timur Rashba. Axions. Originally motivated as a solution to the strong CP problem

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A k- ? model for turbulently thermal convection in solar like and RGB stars

A k- ? model for turbulently thermal convection in solar like and RGB stars. Li Yan Yunnan Astronomical Observatory, CAS. 1. Turbulently thermal convection in stars 2. Basic equations and the mixing length theory 3. k- ? model for stellar turbulent convection

454 views • 28 slides

New and Odds on Globular Cluster Stellar Populations: an Observational Point of View

New and Odds on Globular Cluster Stellar Populations: an Observational Point of View (The Snapshot Database) G.Piotto, I. King, S. Djorgovski and G. Bono, S. Cassisi, M. Catelan, F. De Angeli , G. Meylan, A. Recio Blanco , A. Renzini, M. Rich, I. Saviane, M. Zoccali.

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1.7 Turbulent Flow

1.7 Turbulent Flow. Turbulent flow is characterized by the random and chaotic motion of fluid molecules. 1.7.1 Time-smoothed variables. Figure 1.7-1 referred steady and unsteady laminar and turbulent flows. The velocity refers to that at a fixed position in the fluid.

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ALARO P hysics developments at LACE

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330 views • 20 slides

Steven E. Koch NOAA Research - Forecast Systems Laboratory

Structure and Dynamics of a Dual Bore Event during IHOP as Revealed by Remote Sensing and Numerical Simulation. Steven E. Koch NOAA Research - Forecast Systems Laboratory

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ATON code for stellar evolution

254 views • 13 slides

Turbulence closure problem

Turbulence closure problem. Governing equations for the mean turbulent flow. 10 equations. Simplification of governing equations. Assumptions: a. Mean vertical velocity is zero. Hydrostatic balance is applied.

171 views • 12 slides