Reference: Summary of the Equations of Fluid Dynamics Fluid Mechanics, L.D. Landau & E.M. Lifshitz 1 Introduction Emission processes give us diagnostics with which to estimate important parameters, such as the density, and magnetic field, of an astrophysical plasma. Fluid dynamics provides us with the capability of understanding the transport of mass, momentum and energy. Normally one spends more than a lecture on Astrophysical Fluid Dynamics since this relates to many areas of astrophysics. In following lectures we are going to consider one principal application of astrophysical fluid dynamics accretion discs. Note also that magnetic fields are not included in the following. Again a full treatment of magnetic fields warrants a full course. The fundamental fluid dynamics equations The equations of fluid dynamics are best expressed via conservation laws for the conservation of mass, momentum and energy. Fluid Dynamics 1/
.1 Conservation of mass The continuity equation Since the volume is arbitrary, S Control volume for assessing conservation of mass. n i v i Consider the rate of change of mass within a fixed volume. This changes as a result of the mass flow through the bounding surface. t ρd Using the divergence theorem, ρ ----- t t ρd x i S ρv i n i ds + ( ρvi ) d 0 ρ ----- + ( ρvi ) d 0 t x i + ( ρvi ) 0 Fluid Dynamics /
. Conservation of momentum n i Consider now the rate of change of momentum within a volume. This decreases as a result of the flux of momentum through the bounding surface and increases as the result of body forces (in our case gravity) acting on the volume. Let S Π i n Π i Flux of i component of momentum in the direction and f i Body force per unit mass t then ρvi d Π i n ds + ρ f i d S There is an equivalent way of thinking of Π i, which is often useful, and that is, Π i n ds is the i th component of the force exerted on the fluid exterior to S by the fluid interior to S. Fluid Dynamics 3/
Again using the divergence theorem, ( ρvi ) t + Π i x d ρ f i d ( ρvi ) t + Π i x ρf i Gravity For gravity we use the gravitational potential f i φ G x i For a single gravitating obect of mass M φ G GM --------- r Fluid Dynamics 4/
and for a self-gravitating distribution where G is Newton s constant of gravitation. Expressions for Π i The momentum flux is composed of a bulk part plus a part resulting from the motion of particles moving with respect to the centre of mass velocity of the fluid ( v i ). For a perfect fluid (an approximation often used in astrophysics), we take p to be the isotropic pressure, then The equations of motion are then: ( ρvi ) t φ G 4πGρ φ G G ρ x i ------------------ ( ) x i x i d3x Π i ρv i v + pδ i φ G + ( ρvi v x + pδ i ) ρ xi ( ρvi ) t + x ( ρvi v ) p φ G ρ xi Fluid Dynamics 5/
There is also another useful form for the momentum equation derived using the continuity equation. ( ρvi ) t ρ + ( ρvi v x ) v i t v i v i + ρ + v t i ( ρv x ) + ρv x v i ρ t v i v i + ( ρv x ) + ρ + ρv t x v i v i ρ + ρv t x Hence, another form of the momentum equation is: On dividing by the density v i v i ρ + ρv t x p ------ ρ φ G --------- v i v i + v t x 1 p -- ------ ρ φ G --------- Fluid Dynamics 6/
Differentiation following the motion This is a good place to introduce differentiation following the motion. For a function f following the motion of a fluid element which has coordinates x i x i () t f( x i, t), the variation of is given by: df ----- f + f ------- dxi t f t + v i f x i Hence, the momentum equation can be written compactly as ρ dv i ------ p φ G ρ xi Fluid Dynamics 7/
.3 Thermodynamics m S U p Before going on to consider the consequences of the conservation of energy, we consider the thermodynamics of a comoving volume element. (See the figure at left.) Element of fluid and the variables used to describe its state. Define: m ε P s T Mass of element Internal energy density per unit volume pressure (as above) entropy per unit mass temperature (in degrees Kelvin) Fluid Dynamics 8/
We have the following quantities for the volume element: U Total internal energy S Entropy ms volume The second law of thermodynamics tell us that the change in entropy of a mass of gas is related to changes in other thermodynamic variables as follows: m --- ρ ktds du + pd ktd( ms) d mε ------ + pd m ρ --- ρ ktds d ε ρ -- + pd 1 ρ -- ρktds dε ( ε + p) ----------------dρ ρ 1 --dε ρ mε ------ ρ ( ε + p) ----------------dρ ρ Fluid Dynamics 9/
Specific enthalpy A commonly used thermodynamic variable is the specific enthalpy: In terms of the specific enthalpy, the equation becomes h ε + p ----------- ρ ktds d ε ρ -- + pd 1 ρ -- ktds d ε ----------- + p d p ρ -- + pd 1 ρ ρ -- dh dp ----- ρ For a parcel of fluid following the motion, we obtain, after dividing by the time increment of a volume element, ρkt ds ---- kt ds ---- dε ----- dh ----- ( ε + p) ---------------- dρ ----- ρ 1 -- dp ----- ρ Fluid Dynamics 10/
The fluid is adiabatic when there is no transfer of heat in or out of the volume element: kt ds ---- 0 dε ----- ( ε + p) ---------------- dρ ----- ρ 0 dh 1 ----- -- dp ----- ρ 0 The quantities ds, dε, dp etc. are perfect differentials, and these relationships are valid relations from point to point within the fluid. Two particular relationships we shall use in the following are: s ρkt t s ρkt xi ε t h ρ xi ρ h t p.3.1 Equation of state The above equations can be used to derive the equation of state of a gas in which the ratio of specific heats ( γ c p c v ) is a constant. Consider the following form of the entropy, internal energy, pressure relation: ρktds dε ( ε + p) ----------------dρ ρ Fluid Dynamics 11/
In a perfect gas, p ρkt ---------- µm p where µ is the mean molecular weight and Hence, p ( γ 1)ε ε + p (We can discard the s 0 since the origin of entropy is arbitrary.) γε µm p ( γ 1)εds dε µm p ( γ 1)ds dε ----- ε γε ----dρ ρ γ --dρ ρ µm p ( γ 1) ( s s 0 ) lnε γlnρ ε ----- exp [ µm p ( γ 1) ( s s 0 )] exp[ µm p ( γ 1)s] ρ γ Fluid Dynamics 1/
We therefore have, ε exp[ µm p ( γ 1)s] ρ γ The function K( s) is often referred to as the pseudo-entropy. For a completely ionised monatomic gas γ 5 3..4 Conservation of energy Take the momentum equation in the form: p ( γ 1) exp[ µm p ( γ 1)s] ρ γ K( s)ρ γ and take the scalar product with the velocity: v i v i ρ + ρv t x P ------ ρ φ G --------- v i v i P φ G ρv i + ρv t v i v ------ ρv --------- i ρ 1 --v t i v i ρv 1 --v x i v P φ G + i v i ρv --------- i Fluid Dynamics 13/
That is, ρ 1 --v t ρv 1 --v x p φ G + v i ρv --------- i Before, we used the continuity equation to move the ρ and ρv outside the differentiations. Now we can use the same technique to move them inside and we recover the equation: 1 --ρv t 1 --ρv x v p φ G + v i ρv --------- i The aim of the following is to put the right hand side into some sort of divergence form. Consider first the term P s v i ρktv i h ρv i x i ρkt ds s h ---- ρkt ρv t i ρkt ds ---- ε ρ h + h ρvi t t Fluid Dynamics 14/
ρ We now eliminate the term using continuity, viz t ρ t ( ρvi ) and we obtain p v i ρkt ds ---- x i ε h t ( ρvi ) ρv h xi i x i ρkt ds ---- ε t ( ρhvi ) Fluid Dynamics 15/
The term φ G ρv i x i ( ρφg v ) + φ G ( ρvi ) i x i ρ ( ρφg v i ) φ G t ( ρφg v i ) φ G ( ρφg ) + ρ t t When the gravitational potential is constant in time, φ G φ G 0 ρv t i ( ρφg v i ) ( ρφg ) t Hence, the energy equation 1 --ρv t 1 --ρv x v P φ G + v i ρv --------- i Fluid Dynamics 16/
becomes 1 --ρv t 1 + --ρv x v ρkt ds ---- ε t ( ρφg v i ) ( ρhvi ) ( ρφg ) t Bringing terms over to the left hand side: 1 --ρv t + ε + ρφ G 1 + --ρv x v + ρhv + ρφ G v ρkt ds ---- When the fluid is adiabatic and we have the energy equation for a perfect fluid: ρkt ds ---- 0 1 --ρv t + ε + ρφ G 1 + --ρv x v + ρhv + ρφ G v 0 Fluid Dynamics 17/
The total energy per unit volume is E 1 --ρv + ε + ρφ G Kinetic + internal + gravitational energy and the energy flux is 1 F E, i --ρv v i + ρhv i + ρφ G v i ρ 1 --v + h + φ Kinetic + enthalpy + gravitational fluxes vi 3 Fluids with viscosity In most astrophysical contexts we do not have to consider molecular viscosity since it is generally small. However, we do need to consider viscosity in circumstances where it is important to discuss the means whereby energy is dissipated in a fluid. 3.1 The momentum flux in a viscous fluid The starting point for considering viscosity is the momentum flux. We put Π i ρv i v + pδ i σ i Fluid Dynamics 18/
where, the viscous stress tensor, σ i, is given by The tensor σ i η v i, + v i --δ 3 i v k, k + ζδ v i k, k, ηs i + ζδ i v k, k 1 s i -- v + i, v i, --δ 3 i v k, k is the (trace-free) shear tensor of the fluid and v k, k is the dilation, which is important in compressible fluids. The complete equations of motion are therefore: ( ρvi ) t + x ( ρvi v ) p + σ i x φ G ρ xi Fluid Dynamics 19/
3. Energy conservation If we now take the scalar product of the momentum equation with v i we obtain ρ 1 --v t ρv 1 --v x P φ G + v i ρv x i --------- + i x v i x i that is, the same as before, but with the additional term σ i σ i v i x ( vi σ x i ) v i, σ i Hence the energy equation becomes 1 --ρv t + ε + ρφ G 1 + --ρv x v + ρhv + ρφ G v v i σ i ρkt ds ---- v i, σ i Fluid Dynamics 0/
The quantity v i σ i n is interpreted as the work done on the fluid by the viscous force; hence its appearance with terms that we associate with the energy flux. This is not the full story, however. When there is momentum transport associated with viscosity, there is also a heat flux, q which is often represented as being proportional to the temperature gradient with a heat conduction coefficient κ, i.e. q i T κ xi We then write the full energy equation as 1 --ρv t + ε + ρφ G Conservation of energy is expressed by: 1 + --ρv x v + ρhv + ρφ G v v i σ i + q ρkt ds ---- v i, σ i + q, 1 --ρv t + ε + ρφ G and the entropy changes according to 1 + --ρv x v + ρhv + ρφ G v v i σ i + q 0 ρkt ds ---- v i, σ i q, Fluid Dynamics 1/
The term v i, σ i represents viscous heating and the term q, represents escape of heat from the volume resulting from the heat flux. The viscous heating term can be written: remembering the definition of the shear tensor: σ i v i, ηs i s i + ζv k, k 1 s i -- v + i, v i, --δ 3 i v k, k Fluid Dynamics /