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At least 5 per cent of the massive stars are moving supersonically throughthe interstellar medium (ISM) and are expected to produce a stellar wind bowshock. We explore how the mass loss and space velocity of massive runaway starsaffect the morphology of their bow shocks. We run two-dimensional axisymmetrichydrodynamical simulations following the evolution of the circumstellar mediumof these stars in the Galactic plane from the main sequence to the redsupergiant phase. We find that thermal conduction is an important processgoverning the shape, size and structure of the bow shocks around hot stars, andthat they have an optical luminosity mainly produced by forbidden lines, e.g.[OIII]. The Ha emission of the bow shocks around hot stars originates from neartheir contact discontinuity. The H$\alpha$ emission of bow shocks around coolstars originates from their forward shock, and is too faint to be observed forthe bow shocks that we simulate. The emission of optically-thin radiationmainly comes from the shocked ISM material. All bow shock models are brighterin the infrared, i.e. the infrared is the most appropriate waveband to searchfor bow shocks. Our study suggests that the infrared emission comes from nearthe contact discontinuity for bow shocks of hot stars and from the inner regionof shocked wind for bow shocks around cool stars. We predict that, in theGalactic plane, the brightest, i.e. the most easily detectable bow shocks areproduced by high-mass stars moving with small space velocities.

Models of the circumstellar medium of evolving, massive runaway stars moving through the Galactic plane