Figure 1 - uploaded by Michael De Becker
Content may be subject to copyright.
Snapshots of the gas density in the orbital (x − y) plane from the radiatively-driven winds simulation of η Car at φ = 1.0. At periastron (φ = 1.0) the primary is to the left, and the companion is to the right, of the image centre. The plots show a region of ±2 × 10 15 cm (left panel) and ±5 × 10 14 cm (right panel).
Source publication
Massive stars possess powerful stellar winds. Wind-wind collision in a massive star binary system generates a region of thermalized plasma which may emit prolifically at X-ray wavelengths. Results are presented from 3D adaptive-mesh refinement (AMR) hydrodynamical models which include radiative cooling and the radiative driving of the stellar winds...
Context in source publication
Context 1
... in large-scale simulations (Fig. 1), the inclusion of orbital motion of the stars reduces the impact of radiative inhibition and increases the acquired pre-shock velocities. As such, the post- shock gas temperature and cooling time see a commensurate increase, and sufficient gas pressure is preserved to stabilize the WCR against catastrophic instability ...
Similar publications
Context. Massive star winds are known to be responsible for X-ray emission arising from wind plasma heated by the strong shocks up to temperatures of 10 ⁶ –10 ⁷ K in the case of colliding wind binaries. The investigation of X-ray emission from massive stars thus constitutes a valuable tool for identifying binaries, which is otherwise a difficult ta...
