Journal ArticleDOI
Interstellar bubbles. II - Structure and evolution
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In this article, the detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented, including the effects of thermal conduction between the hot interior and the cold shell of swept-up interstellar matter.Abstract:
The detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented. First, an adiabatic similarity solution is given which is applicable at early times. Second, a similarity solution is derived which includes the effects of thermal conduction between the hot (about 1 million K) interior and the cold shell of swept-up interstellar matter. This solution is then modified to include the effects of radiative energy losses. The evolution of an interstellar bubble is calculated, including the radiative losses. The quantitative results for the outer-shell radius and velocity and the column density of highly ionized species such as O VI are within a factor 2 of the approximate results of Castor, McCray, and Weaver (1975). The effect of stellar motion on the structure of a bubble, the hydrodynamic stability of the outer shell, and the observable properties of the hot region and the outer shell are discussed.read more
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The effect of stellar winds on the formation of a protocluster
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Radiation-hydrodynamic models of the evolving circumstellar medium around massive stars
Jesús A. Toalá,Sarah Jane Arthur +1 more
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Journal ArticleDOI
Disruption of the Orion molecular core 1 by wind from the massive star θ 1 Orionis C
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TL;DR: This finding demonstrates that the mechanical energy from the stellar wind is converted very efficiently into kinetic energy of the shell and causes more disruption of the Orion molecular core 1 than do photo-ionization and evaporation or future supernova explosions.
Journal ArticleDOI
Superbubbles in the Multiphase ISM and the Loading of Galactic Winds
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Journal ArticleDOI
Structure of the region of solar wind—Interstellar medium interaction and its influence on H atoms penetrating the solar wind
TL;DR: The structure of the region of interaction between the solar wind and the interstellar medium in the two-shocks model (TSM) was numerically calculated by Baranovet et al. as discussed by the authors.