Bow shocks, bow waves, and dust waves - I. Strong coupling limit
Abstract
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 cm^{-3}. At higher densities radiation-supported bow shells 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 bow shells become more prevalent.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- July 2019
- DOI:
- 10.1093/mnras/stz1043
- arXiv:
- arXiv:1903.03737
- Bibcode:
- 2019MNRAS.486.3423H
- Keywords:
-
- circumstellar matter;
- stars: winds;
- outflows;
- Astrophysics - Solar and Stellar Astrophysics;
- Astrophysics - Astrophysics of Galaxies
- E-Print:
- 10 pages, 8 figures, MNRAS accepted (revisions: Fig 5 split into 3 parts and captions expanded