Titlebook: Hydrodynamics and Stellar Winds; An Introduction Walter J. Maciel Textbook 2014 Springer Nature Switzerland AG 2014 Astrophysical fluid equ

Diuretic

吵鬧

The Continuity Equation,This chapter discusses the continuum hypothesis, and presents the continuity equation, which is written in spherical and cylindrical coordinates. The chapter ends with a discussion of the mass loss rate as related to the continuity equation. Several examples are worked out, involving the loss of mass in hot and cool stars.

不合

The Equation of State,This chapter introduces the equation of state, defines the mean molecular weight, discusses the validity of the perfect gas hypothesis, and presents several examples regarding stellar photospheres.

Tartar

Gossamer

Cartesian Tensor Notation,This chapter presents the Cartesian tensor notation, or index notation, and shows how the main vector operations can be written in this notation.

綠州

Fluid Equations in Tensor Form,This chapter presents the main fluid equations, namely the continuity, Euler and energy equations using the Cartesian tensor notation. The momentum flux tensor is defined in the framework of the Euler equation in the presence of external forces.

過份好問

The Navier-Stokes Equation,The main goal of this chapter is to present the Navier-Stokes equation, both for incompressible and compressible fluids. The equation is written in the cartesian tensor notation and also in the usual vector form. The viscosity and rate of strain tensors are introduced, as well as the viscosity coefficients.

駭人

讓步

Stellar Winds: An Overview,This chapter presents a general view of stellar winds, the main observational evidences and driving mechanisms. An estimate is made of the mass loss rates for hot and cool stars. The chapter ends with some comments on the interaction of the winds with the interstellar medium and the effects of winds on the evolution of the stars.

強有力

978-3-319-04327-2Springer Nature Switzerland AG 2014