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Bow shocks, bow waves, and dust waves. I. Strong coupling limit
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Dust waves and bow waves result from the action of a star's radiation pressure on a stream of dusty plasma that flows past it. They are an alternative mechanism to hydrodynamic bow shocks for explaining the curved arcs of infrared emission seen around some stars. When gas and grains are perfectly coupled, for a broad class of stellar parameters, wind-supported bow shocks predominate when the ambient density is below 100 per cubic cm. At higher densities radiation-supported bows can form, tending to be optically thin bow waves around B stars, or optically thick bow shocks around early O stars. For OB stars with particularly weak stellar winds, radiation-supported bows become more prevalent.
Forward citations
Cited by 2 Pith papers
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An Halpha survey of infrared bow-shocks around OB-type stars
Fifteen plus one serendipitous clear H-alpha bow shocks are detected among 78 IR candidates; several are consistent with radiation-supported regimes while others match classical wind-supported shocks.
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Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry
Bulk interstellar gas motion, not stellar motion, dominates most massive star bow shocks; only about 21% are classical aligned bow shocks.
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