AbstractThe problem of a cold gas flowing past an unmovable object is considered. It is shown that at large distances from the obstacle the shock front forms a parabolic body of revolution. The interior of the shock front is obtained by solution of the hydrodynamic equations in parabolic coordinates. The results are verified with a hydrodynamic simulation. Finally, relations to astrophysical bow shocks and other analytical works on oblique shocks is discussed.

Bow shocks occur when a supersonic flow encounters an obstacle. A prominent example from astrophysics is planetary bow shocks(Treumann 2008). Another common astrophysical scenario where shock waves emerge is when supernova remnants engulf a dense molecular cloud (McKee 1975). A bow shock has even been observed around a star that moves supersonically relative to the ISM (Noriega-Crespo 1997).

Bow shocks have been studied extensively, both theoretically (Wilkin 1996, Farris 1994) and numerically (Mohamed 2012, Miceli 2006). However, all studies were carried out under the assumption of finite Mach number. In this work we rather assume that the incoming matter is cold, so for every finite velocity its Mach number would be infinite. The asymptotic shape far from the obstacle is qualitatively different between the two. In the case of a finite Mach number \(M\), far away from the obstacle the length scale of the obstacle becomes irrelevant, and the shock front coincides with the Mach cone, i.e. a cone with an opening angle \(\alpha=\sin^{-1}\frac{1}{M}\) (LANDAU 1987). However, as we shall later see, in the case of an infinite Mach number, the shock front is parabolic solid of revolution. For a spherical obstacle of radius \(R_{o}\), the shock front loci in cylindrical coordinates is \(z=\xi\frac{r^{2}}{R_{o}}\), where \(\xi\) is a dimensionless constant. This means that no matter how far from the obstacle, the obstacle’s length scale is never negligible. For a very large Mach number, we should expect that the transition from former to the later should occur where the two curves intersect

\begin{equation}
r_{t}\approx R_{o}\sqrt{M^{2}-1}\\
\end{equation}

\begin{equation}
z_{t}\approx R_{o}\left(M^{2}-1\right)\\
\end{equation}

The solution described here is asymptotic, which means it is only valid at distances much larger than the obstacle. This means that the solution can only manifest itself high Mach number flows, and even then, it would only occupy the region \(zM^{2}>z\gg R_{o}\).

This paper is organized as follows. In section 2 we describe the complete mathematical formulation. In section 3 we present validation of our analytic results with a numerical simulation. Finally, in section 4, we discuss the results.

Spherical parabolic coordinates are given by

\begin{equation}
x=\sigma\tau\cos\phi\\
\end{equation}

\begin{equation}
y=\sigma\tau\sin\phi\\
\end{equation}

\begin{equation}
z=\frac{1}{2}\left(\tau^{2}-\sigma^{2}\right)\\
\end{equation}

In these coordinates, the steady state, azimuthally symmetric hydrodynamics equations take the following form. The conservation of mass is

\begin{equation}
\frac{\partial}{\partial\sigma}\left(\sqrt{\sigma^{2}+\tau^{2}}\sigma\tau v_{\sigma}\right)+\frac{\partial}{\partial\tau}\left(\sqrt{\tau^{2}+\sigma^{2}}\sigma\tau v_{\tau}\right)=0\\
\end{equation}

The conservation of entropy is

\begin{equation}
v_{\sigma}\frac{\partial s}{\partial\sigma}+v_{\tau}\frac{\partial s}{\partial\tau}=0\\
\end{equation}

where \(s=\ln p-\gamma\ln\rho\) is the specific entropy. The conservation of momentum in each direction is

\begin{equation}
v_{\sigma}\frac{\partial v_{\sigma}}{\partial\sigma}+v_{\tau}\frac{\partial v_{\sigma}}{\partial\tau}+\frac{v_{\tau}\left(v_{\sigma}\tau-v_{\tau}\sigma\right)}{\tau^{2}+\sigma^{2}}+\frac{1}{\rho}\frac{\partial p}{\partial\sigma}=0\\
\end{equation}

\begin{equation}
v_{\sigma}\frac{\partial v_{\tau}}{\partial\sigma}+v_{\tau}\frac{\partial v_{\tau}}{\partial\tau}-\frac{v_{\sigma}\left(v_{\sigma}\tau-v_{\tau}\sigma\right)}{\tau^{2}+\sigma^{2}}+\frac{1}{\rho}\frac{\partial p}{\partial\tau}=0\\
\end{equation}

One of the momentum equations can be replaced by Bernoulli’s equation

\begin{equation}
\frac{1}{2}v_{in}^{2}=\frac{1}{2}v_{\sigma}^{2}+\frac{1}{2}v_{\tau}^{2}+\frac{1}{\gamma-1}c^{2}\\
\end{equation}

where \(c\) is the speed of sound. We found it most convenient to express the equations in terms of the density \(\rho\), the sound speed \(c\), and the two Mach numbers \(m_{\sigma,\tau}=\frac{v_{\sigma,\tau}}{c}\)

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