Refraction from interstellar shocks

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Abstract
Interstellar shocks that are sufficiently thin (≲10 au) and sufficiently strong (ΔD M≳0.01 cm− 3 pc) are capable of producing observable flux modulations and multiple images of background point radio sources. From the statistics of observed refraction events, inferences may be drawn concerining the relationship between small‐scale electron density structure and large‐scale phenomena like supernova explosions and strong stellar winds. In order for shock refraction events to be frequent, the effective cross section must be much larger than predicted for an ideal, spherical shock. The cross section is likely to be enhanced by turbulence that distorts the shock interface on scales of ∼1 au and by the prevalence of HI clouds and other non‐uniformities in the ISM that will be swept up or engulfed by the expanding blast wave.

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