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- W2101967595 abstract "At least 5 per cent of the massive stars are moving supersonically through the interstellar medium (ISM) and are expected to produce a stellar wind bow shock. We explore how the mass loss and space velocity of massive runaway stars affect the morphology of their bow shocks. We run two-dimensional axisymmetric hydrodynamical simulations following the evolution of the circumstellar medium of these stars in the Galactic plane from the main sequence to the red supergiant phase. We find that thermal conduction is an important process governing the shape, size and structure of the bow shocks around hot stars, and that 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 near their contact discontinuity. The H$alpha$ emission of bow shocks around cool stars originates from their forward shock, and is too faint to be observed for the bow shocks that we simulate. The emission of optically-thin radiation mainly comes from the shocked ISM material. All bow shock models are brighter in the infrared, i.e. the infrared is the most appropriate waveband to search for bow shocks. Our study suggests that the infrared emission comes from near the contact discontinuity for bow shocks of hot stars and from the inner region of shocked wind for bow shocks around cool stars. We predict that, in the Galactic plane, the brightest, i.e. the most easily detectable bow shocks are produced by high-mass stars moving with small space velocities." @default.
- W2101967595 created "2016-06-24" @default.
- W2101967595 creator A5001432824 @default.
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- W2101967595 creator A5078350988 @default.
- W2101967595 date "2014-09-12" @default.
- W2101967595 modified "2023-09-27" @default.
- W2101967595 title "Models of the circumstellar medium of evolving, massive runaway stars moving through the Galactic plane" @default.
- W2101967595 cites W1964548291 @default.
- W2101967595 cites W1974222442 @default.
- W2101967595 cites W1975207394 @default.
- W2101967595 cites W1975983552 @default.
- W2101967595 cites W1977121138 @default.
- W2101967595 cites W1988567899 @default.
- W2101967595 cites W1993230081 @default.
- W2101967595 cites W1996312982 @default.
- W2101967595 cites W1997743109 @default.
- W2101967595 cites W1998862619 @default.
- W2101967595 cites W2001586164 @default.
- W2101967595 cites W2006869439 @default.
- W2101967595 cites W2007857565 @default.
- W2101967595 cites W2013285588 @default.
- W2101967595 cites W2018590189 @default.
- W2101967595 cites W2022109855 @default.
- W2101967595 cites W2023056656 @default.
- W2101967595 cites W2024135564 @default.
- W2101967595 cites W2024936798 @default.
- W2101967595 cites W2026755197 @default.
- W2101967595 cites W2035965985 @default.
- W2101967595 cites W2038274723 @default.
- W2101967595 cites W2044257729 @default.
- W2101967595 cites W2047047228 @default.
- W2101967595 cites W2050435264 @default.
- W2101967595 cites W2050547342 @default.
- W2101967595 cites W2052356736 @default.
- W2101967595 cites W2055667453 @default.
- W2101967595 cites W2063437365 @default.
- W2101967595 cites W2063451176 @default.
- W2101967595 cites W2067886648 @default.
- W2101967595 cites W2071700939 @default.
- W2101967595 cites W2072479916 @default.
- W2101967595 cites W2073084532 @default.
- W2101967595 cites W2075705929 @default.
- W2101967595 cites W2077310516 @default.
- W2101967595 cites W2080704047 @default.
- W2101967595 cites W2083857106 @default.
- W2101967595 cites W2086252387 @default.
- W2101967595 cites W2089390834 @default.
- W2101967595 cites W2092770211 @default.
- W2101967595 cites W2096177980 @default.
- W2101967595 cites W2102467331 @default.
- W2101967595 cites W2102470784 @default.
- W2101967595 cites W2102658716 @default.
- W2101967595 cites W2108490226 @default.
- W2101967595 cites W2109706536 @default.
- W2101967595 cites W2109993551 @default.
- W2101967595 cites W2129830851 @default.
- W2101967595 cites W2132178729 @default.
- W2101967595 cites W2135785862 @default.
- W2101967595 cites W2139741136 @default.
- W2101967595 cites W2140888726 @default.
- W2101967595 cites W2144175537 @default.
- W2101967595 cites W2151733113 @default.
- W2101967595 cites W2153451717 @default.
- W2101967595 cites W2164016695 @default.
- W2101967595 cites W2166776024 @default.
- W2101967595 cites W2394881825 @default.
- W2101967595 cites W2899497983 @default.
- W2101967595 cites W2949821474 @default.
- W2101967595 cites W3014299595 @default.
- W2101967595 cites W3041140614 @default.
- W2101967595 cites W3098467601 @default.
- W2101967595 cites W3098691340 @default.
- W2101967595 cites W3098876131 @default.
- W2101967595 cites W3099985757 @default.
- W2101967595 cites W3102318835 @default.
- W2101967595 cites W3102660983 @default.
- W2101967595 cites W3104291191 @default.
- W2101967595 cites W3104929225 @default.
- W2101967595 cites W3105647200 @default.
- W2101967595 cites W3121503080 @default.
- W2101967595 cites W3124032753 @default.
- W2101967595 cites W3124706624 @default.
- W2101967595 cites W4213233494 @default.
- W2101967595 cites W4234270804 @default.
- W2101967595 cites W4293227712 @default.
- W2101967595 cites W4293228180 @default.
- W2101967595 cites W4297430188 @default.
- W2101967595 cites W4299444469 @default.
- W2101967595 cites W4300952231 @default.
- W2101967595 doi "https://doi.org/10.1093/mnras/stu1629" @default.
- W2101967595 hasPublicationYear "2014" @default.
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