Eliminating Pressure for Incompressible MHD
March 27, 2026·
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1 min read
Xinyu Li
In the formulation of Elsasser’s variables $\mathbf{U} = \mathbf{v}+\mathbf{b}$ and $\mathbf{W} = \mathbf{v}-\mathbf{b}$,
$$\begin{aligned} &&\partial_t \mathbf{U} = -(\mathbf{W}\cdot\nabla)\mathbf{U}-\nabla p,\\ &&\partial_t \mathbf{W} = -(\mathbf{U}\cdot\nabla)\mathbf{W}-\nabla p,\\ &&\nabla\cdot\mathbf{U} = \nabla\cdot\mathbf{W} = 0. \end{aligned}$$For undisturbed fluid $\mathbf{U} = V_A$ and $\mathbf{W} =- V_A$. Introducing small purturbation $\mathbf{U} = V_A+\mathbf{u}$ and $\mathbf{W} = -V_A+\mathbf{w}$
$$\begin{aligned} &&\partial_t\mathbf{u}-V_A\partial_z\mathbf{u} = -(\mathbf{w}\cdot\nabla)\mathbf{u}-\nabla p,\\ &&\partial_t\mathbf{w}+V_A\partial_z\mathbf{w} = -(\mathbf{u}\cdot\nabla)\mathbf{w}-\nabla p.\\ \end{aligned}$$Taking the divergence of above equations
$$\begin{aligned} \nabla p = \nabla\cdot[(\mathbf{w}\cdot\nabla)\mathbf{u}]. \end{aligned}$$In the Fourier space
$$\begin{aligned} k^2 \tilde{p} = (\mathbf{k}\cdot\tilde{\mathbf{u}}(\mathbf{k}_1))(\mathbf{k}_1\cdot\tilde{\mathbf{w}}(\mathbf{k}_2))\delta(\mathbf{k}_1+\mathbf{k}_2-\mathbf{k}). \end{aligned}$$Therefore the Fourier transformation of $\nabla p $ gives
$$\begin{aligned} \mathbf{k}p = (\hat{\mathbf{k}}\cdot\tilde{\mathbf{u}}(\mathbf{k}_1))(\mathbf{k}\cdot\tilde{\mathbf{w}}(\mathbf{k}_2))\delta(\mathbf{k}_1+\mathbf{k}_2-\mathbf{k}), \end{aligned}$$where the incompressible condition $\mathbf{k}_2\cdot\tilde{\mathbf{w}}(\mathbf{k}_2)=0$ is used.
Taking the Fourier transform of the perturbed equations and defining $\omega_k = V_A k_z$
$$\begin{aligned} &&(\partial_t-i\omega_k)\tilde{\mathbf{u}}(\mathbf{k}) = -\frac{i}{8\pi}\int d^3 k_1 d^3 k_2\:[\tilde{\mathbf{u}}(\mathbf{k}_1)-\hat{\mathbf{k}}(\hat{\mathbf{k}}\cdot\tilde{\mathbf{u}}(\mathbf{k}_1)](\mathbf{k}\cdot\tilde{\mathbf{w}}(\mathbf{k}_2))\delta(\mathbf{k}_1+\mathbf{k}_2-\mathbf{k})\\ &&(\partial_t-i\omega_k)\tilde{\mathbf{w}}(\mathbf{k}) = -\frac{i}{8\pi}\int d^3 k_1 d^3 k_2\:[\tilde{\mathbf{w}}(\mathbf{k}_1)-\hat{\mathbf{k}}(\hat{\mathbf{k}}\cdot\tilde{\mathbf{w}}(\mathbf{k}_1)](\mathbf{k}\cdot\tilde{\mathbf{u}}(\mathbf{k}_2))\delta(\mathbf{k}_1+\mathbf{k}_2-\mathbf{k}) \end{aligned}$$
Authors
Assistant Professor
Xinyu Li is an assistant professor in the Department of Astronomy, Tsinghua University. He is fond of discovering fundamental physical laws from the vast observation of various astrophysical objects. His research areas are high energy astrophysics, plasma astrophysics and cosmology. His research topics cover a broad range of physical scales: from the smallest fundamental particles like electrons and ultralight axions, to neutron stars, black holes and galaxies, and to the largest scale structure of the universe.