Conservation Laws in Ideal MHD

Transcription

1 Conservation Laws in Ideal MHD Nick Murphy Harvard-Smithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics February 3, 2016 These lecture notes are largely based on Plasma Physics for Astrophysics by Russell Kulsrud, Lectures in Magnetohydrodynamics by the late Dalton Schnack, Ideal Magnetohydrodynamics by Jeffrey Freidberg, Magnetic Reconnection by Eric Priest and Terry Forbes, and various papers by M. Berger & J. Perez. The description of Stokes Theorem and the Divergence Theorem come from Stewart s Multivariable Calculus with figures adapted from Wikimedia Commons and R. Fitzpatrick s online notes.

2 Outline Mathematical interlude: Stokes Theorem Divergence Theorem Dyadic tensors Conservation of mass, momentum, and energy The frozen-in condition Helicity and cross-helicity

3 Stokes Theorem Let S be an oriented piecewise-smooth surface that is bounded by a simple, close, piecewise-smooth boundary curve C with positive orientation. Let F be a vector field whose components have continuous partial derivatives on an open region in R 3 that contains S. Then F dr = F ds (1) C where ds = ˆn ds and ˆn is a unit normal vector to S S

4 The Divergence Theorem (also called Gauss s Theorem) Let V be a simple solid region and let S be the boundary surface of V, given with positive (outward) orientation. Let F be a vector field whose component functions have continuous partial derivatives on an open region that contains V. Then F ds = F dv (2) S The interior contributions to the divergence integral cancel, so only the exterior contributions remain V

5 While somewhat horrible, dyadic tensors 1 allow the equations of MHD to be written in a compact/useful form A dyadic tensor is a second rank tensor that can be written as the tensor product of two vectors: A ij = B i C j A = BC = (B 1 ê 1 + B 2 ê 2 + B 3 ê 3 ) (C 1 ê 1 + C 2 ê 2 + C 3 ê 3 ) = B 1 C 1 ê 1 ê 1 + B 1 C 2 ê 1 ê 2 + B 1 C 3 ê 1 ê 3 + B 2 C 1 ê 2 ê 1 + B 2 C 2 ê 2 ê 2 + B 2 C 3 ê 2 ê 3 + B 3 C 1 ê 3 ê 1 + B 3 C 2 ê 3 ê 2 + B 3 C 3 ê 3 ê 3 (3) where ê 1... are unit vectors and ê 1 ê 3... are unit dyads, e.g.: ê 1 ê 3 = (4) Good resources: Lectures in Magnetohydrodynamics by Dalton Schnack and rect.html

6 Dot products and double dot products with dyadic tensors In general, BC CB Dot products from the left and right are different: ê 1 A = B 1 C 1 ê 1 + B 1 C 2 ê 2 + B 1 C 3 ê 3 (5) A ê 1 = B 1 C 1 ê 1 + B 2 C 1 ê 2 + B 3 C 1 ê 3 (6) Double-dot notation is ambiguous but we use: A : T A ij T ij where we sum over repeated indices

7 The divergence of a dyadic tensor is a vector The divergence of a dyadic tensor is This is a vector whose jth component is T = i T ij (7) ( T) j = T 1j x 1 + T 2j x 2 + T 3j x 3 (8) We can even generalize Gauss theorem! T dv = ds T (9) S

8 What about the dyad T V? The gradient operator is given by ê i ê 1 + ê 2 + ê 3 (10) x i x 1 x 2 x 3 Then T V is given in Cartesian coordinates by ( V) ij = V j x i (11) V = V j ê i ê j (12) x i x V x x V y x V z = y V x y V y y V z (13) z V x z V y z V z where i is the row index and j is the column index

9 Conservative form As mentioned previously, conservative form is usually given by (stuff) + (flux of stuff) = 0 (14) t where source and sink terms go on the RHS If stuff is a scalar, then flux of stuff is a vector If stuff is a vector, then flux of stuff is a dyadic tensor If Eq. 14 is satisfied, then stuff is locally conserved

10 The continuity equation is already in conservative form The continuity equation 2 is ρ t where ρv is the mass flux + (ρv) = 0 (15) Mass is locally conserved the universe is safe once again! 2 This expression is similar to the Law of Conservation of Space Wombats

11 Is mass conserved globally? Integrate the continuity equation over a closed volume V bounded by a surface S [ ] ρ V t + (ρv) dv = 0 (16) ρ dv + (ρv) dv = 0 (17) t V V Now define M as the mass within V and use Gauss theorem dm + ds (ρv) = 0 (18) }{{} dt S }{{} change of mass in V mass flow through S Yep, we re still good. Mass is conserved globally. Recall that this was how we derived the continuity equation in the first place!

12 The momentum equation in conservative form The momentum equation can be written as ρv t + T = 0 (19) where the ideal MHD stress tensor T is ) T = ρvv + (p + B2 I BB 8π 4π and I ê 1 ê 1 + ê 2 ê 2 + ê 3 ê 3 is the identity dyadic tensor The quantity p + B 2 /8π is the total pressure (20) One can also include the viscous and gravitational stress tensors, or use a pressure tensor rather than a scalar pressure

13 Physical meaning of the stress tensor Imagine you have an infinitesimal box Forces are exerted on each face by the outside volume The forces on each side of the box could have components in three directions The stress tensor includes the nine quantities needed to describe the total force exerted on this box

14 The Reynolds stress tensor The Reynolds stress is given by T V ρvv (21) T V represents the flux of momentum. Think: T V ρv }{{} Momentum density V }{{} times a velocity (22) (ρv x )V y is the rate at which the x component of momentum is carried in the y direction (and vice versa)

15 The Maxwell stress tensor The Maxwell stress is T B B2 8π I BB 4π Momentum is transported by the magnetic field The quantity BB 4π motions is the hoop stress which resists shearing (23)

16 We can t always drop gravity! (Kulsrud, p. 77) Gravity is often treated as a body force where g is constant More generally, g is found using the gradient of a scalar potential, φ, g = φ (24) where Poisson s equation is used to solve for the potential, The gravitational stress tensor is 2 φ = 4πGρ (25) T g = ( φ)2 I 8πG where φ φ is a dyadic tensor φ φ 4πG The usual form of the force may be recovering using (26) ρg = T g (27)

17 CGL theory allows for p p For a scalar pressure, the corresponding part of the stress tensor is symmetric p 0 0 T p = pi = 0 p 0 (28) 0 0 p Chew, Goldberger, & Low (1956) allow for different perpendicular and parallel pressures in the double adiabatic approximation T CGL = p p p (29) Used more frequently in astrophysics than in laboratory or space plasma physics

18 Conservation of energy The energy equation can be written as The energy density is w t + s = 0 (30) The energy flux is w = ρv 2 }{{} 2 kinetic + B2 8π }{{} magnetic + p γ 1 }{{} internal (31) s = ρv 2 2 V + p }{{} γ 1 V }{{} kinetic internal + pv }{{} work + ce B 4π }{{} Poynting (32) pv represents the work done on the plasma from p forces

19 We now have a set of three equations describing conservation of mass, momentum, and energy Conservation of mass, momentum, & energy are given by ρ + (ρv) t = 0 (33) ρv + T t = 0 (34) w t + s = 0 (35) where the stress tensor, energy density, and energy flux are ) T = ρvv + (p + B2 I BB (36) 8π 4π w = ρv B2 8π + p (37) γ 1 ( ρv 2 s = 2 + γ ) γ 1 p V + E B (38) 4π

20 The most important property of ideal MHD is the frozen-in condition Define S as a surface bounded by a closed curve C that is co-moving with the plasma The magnetic flux through S is Ψ = B ds (39) There are contributions to dψ dt from: Changes in B with S held fixed, dψ1 dt The flux swept out by C as it moves with the plasma, dψ 2 dt S

21 How does the flux change due to B changing? Take the time derivative of the magnetic flux with S fixed: dψ 1 B = dt S t ds = c ( E) ds S = c E dl (40) where we used Faraday s law and Stokes theorem. C

22 How does the area of S change as it is swept with the plasma? C 2 V ds dl C 1 The lateral area swept out by C as it flows with the plasma is ds = Vdt dl (41) where the line element dl is tangent to C The flux through this area is B ds = B Vdt dl, so that dψ 2 = B V dl dt C = V B dl (42) C

23 Putting it all together The total change in magnetic flux through S is then dψ dt But E + V B c = dψ 1 + dψ 2 dt dt = c E dl C }{{} changes in B = c C ( E + V B c = 0 in ideal MHD, so that V B dl C }{{} changes in S ) dl (43) dψ dt = 0. (44) The magnetic flux through any co-moving fluid element remains constant in ideal MHD.

24 In ideal MHD, the magnetic field and plasma are frozen-in to each other If a parcel of plasma moves, the magnetic field attached to the parcel moves along with it More rigorously: if two plasma elements are initially connected by a magnetic field line, they will remain connected by a magnetic field line at future times. Magnetic topology (e.g., connectivity) is preserved in ideal MHD The plasma cannot move across magnetic field lines (though it remains free to move along field lines)

25 A useful concept in ideal MHD is a field line velocity More generally, flux will be frozen-in if there exists some velocity U such that E + U B c = 0 (45) The velocity U is a field line velocity. In ideal MHD, U is the bulk fluid velocity V A field line velocity does not need to be a fluid velocity In Hall MHD, the field line velocity is the electron velocity

26 What is meant by a field line velocity? In ideal MHD, a key field line velocity is V = c E B B 2 (46) This is the component of velocity perpendicular to B that the plasma is traveling at which is frozen into B The concept of a field line velocity is frought with peril. There is no way to distinguish one field line from another at different times There are an infinite number of field line velocities U is arbitrary (but in ideal MHD we usually pick V )

27 Eyink et al. (2013) argue that stochastic field line wandering in turbulence leads to Richardson diffusion that breaks down the frozen-in condition This result warrants further investigation by independent groups

28 Magnetic helicity measures the linkage of magnetic fields The magnetic field B can be written in terms of a vector potential B = A (47) while noting that A is not gauge invariant: A = A + φ The helicity of a magnetic field is given by H = A B dv (48) V A B should not be considered a helicity density because of gauge freedom! Helicity is approximately conserved during magnetic reconnection and topology changes Helicity can be injected into a system such as the solar corona. When too much builds up, helicity ends up being expelled through coronal mass ejections.

29 Helicity examples A single untwisted closed flux loop has H = 0 A single flux rope with a magnetic flux of Φ that twists around itself T times has a helicity of H = T Φ 2 Two interlinked untwisted flux loops with fluxes Φ 1 and Φ 2 have H = ±2Φ 1 Φ 2 where the sign depends on the sense of the linkedness

30 There are generalizations to allow for gauge-invariant definitions of helicity Berger & Field (1984) defined the relative magnetic helicity to be H = (A B A 0 B 0 ) dv (49) V where B 0 = A 0 is the potential field inside V with the same field outside of V (see also Finn & Antonsen 1985) In toroidal laboratory experiments, it is natural to consider the volume contained within conducting wall boundaries that are coincident with closed flux surfaces (i.e., the magnetic field along the wall is parallel to the boundary)

31 Helicity changes through parallel electric fields and helicity being added/removed to system The time evolution of magnetic helicity is given by dh dt = 2c E B dv + 2c A p E ds (50) V S where we choose A p = 0 and A p ds = 0 on S The first term represents helicity dissipation when E 0 But in ideal MHD, E = 0! The second term represents helicity fluxes in and out of system Flux emergence from the solar photosphere corresponds to helicity injection in the corona Helicity injection in laboratory experiments [e.g., the Steady Inductive Helicity Injected Torus (HIT-SI)]

32 The cross helicity H C measures the imbalance between interacting waves (important in MHD turbulence) The cross helicity is given by H C = In ideal MHD, the rate of change of H C is [( dh C 1 = ds dt S 2 V 2 + γ γ 1 V V B dv (51) ) ] p B V (V B) ρ (52) This vanishes when ds B = ds V = 0 along the boundary S or when the boundary conditions are periodic. Cross helicity is an ideal MHD invariant when this integral vanishes

33 Summary Ideal MHD conserves mass, momentum, and energy (as it darn well should!) In ideal MHD, the magnetic field is frozen-in to the plasma flow It is often useful to think in terms of a magnetic field line velocity, but there are caveats! Helicity and cross-helicity provide two topological constraints that are conserved in ideal MHD