SISSI: Supernovae in a stratified, shearing interstellar medium - I. The geometry of supernova remnants

Open Access

Fig. C.3.

Deformation timescale as a function of size. Spheres are deformed greatly after ∼6.5 percent of $t_{orb} (\bar{R})$ $t_{\text{orb}}\left(\bar{R}\right)$ , where $\bar{R} = p R_{0} + (1 - p) (R_{0} - r_{0})$ $\bar{R} = pR_{0} + (1-p)\left(R_{0} - r_{0}\right)$ is a characteristic radius lying between R₀ − r₀ and R₀. Our linear fit yields p ∼ 0.65.

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