Ionizing cylindrical shock in a rotating self-gravitating dusty gas with magnetized isothermal flow

What is it about?

This article analyzes ionizing cylindrical magnetogasdynamic (MGD) shock waves in a rotating, axisymmetric, self-gravitating dusty gas under isothermal conditions. Using Sakurai’s power-series method, closed-form similarity solutions are derived up to the first-order approximation in terms of $\left(\frac{\mathcal{C}}{\mathcal{U}}\right)^2$, where $\mathcal{U}$ is the shock velocity and $\mathcal{C}$ is the sound speed. The ambient medium ahead of the shock is assumed to have power-law variations in density, magnetic pressure, and azimuthal and axial velocities. A detailed parametric study highlights how factors such as the adiabatic index $\gamma$, dust loading $\kappa_p$, gravitational parameter $\mathcal{G}_0$, Shock Cowling index $\mathrm{C}^\star$, rotational parameter $\frac{v_\star}{\mathcal{A}}$, and density variation index $q$ influence the flow and disturbance energy. The velocity–distance and distance–time profiles confirm the decaying nature of the cylindrical shock. These results provide a valuable benchmark for validating self-similar and numerical solutions, offering novel insights into dusty MGD shocks in astrophysical settings such as supernova remnants, protostellar jets, and galactic outflows.

Featured Image

Photo by NASA Hubble Space Telescope on Unsplash

Photo by NASA Hubble Space Telescope on Unsplash