Rapid dissipation of magnetic energy in highly magnetized environments around neutron stars and black holes is a key open question in high-energy astrophysics. We develop a general …
Binary black holes (BBHs) in gaseous medium, such as active galactic nucleus (AGN) disks, are important gravitational-wave sources, yet the gas-driven torque that governs their …
Ultra-faint dwarf galaxies serve as powerful testing grounds for wave dark matter models through dynamical stellar heating. Previous simulation-based work derived a lower bound on …
The energy momentum tensor for a relativistic pressureless fluid is $$T^{\mu\nu} = (\rho h + \frac{b^2}{4\pi})u^\mu u^\nu + \frac{b^2}{8\pi}g^{\mu\nu} - \frac{b^\mu …
Particle Motion in Uniform Perpendicular Electromagnetic Fields A test particle with mass $m$ and charge $q$ moving at velocity $\boldsymbol{v}$ in an electromagnetic field feels …
Consider the ideal incompressible MHD wave governed by the equations $$\begin{aligned} \frac{\partial \vec{v}}{\partial t}+\vec{v}\cdot \nabla\vec{v}&=&\vec{B}\cdot\nabla\vec{B}\\ …
In relativistic MHD, the magnetic field 4-vector $b_\mu$ and electric field $e_\mu$ in the fluid frame is defined through the 4-vector $u^{\mu}$ and EM 2-form $F_{\mu\nu}$.
In the formulation of Elsasser’s variables $\mathbf{U} = \mathbf{v}+\mathbf{b}$ and $\mathbf{W} = \mathbf{v}-\mathbf{b}$, $$\begin{aligned} &&\partial_t \mathbf{U} = …
The fluid equations in the conservative form are $$\begin{aligned} \partial_t \rho +\nabla\cdot(\rho \boldsymbol{u})&=&0 \\ \partial_t (\rho u^i)+\nabla\cdot(\rho …
First image of supermassive black hole binary.