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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Possible detection of O VI from the large magellanic cloud superbubble N70
TL;DR: In this article, Far Ultraviolet Spectroscopic Explorer (FUSE) observations toward four stars in the Large Magellanic Cloud (LMC) superbubble N70 and compare these spectra to those of four comparison targets located in nearby field and diffuse regions.
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The energetics and mass loss of the dwarf starburst Markarian 33
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Journal ArticleDOI
A Large H I Shell surrounding the Wolf-Rayet Star HD 191765
Simon Gervais,Nicole St-Louis +1 more
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Journal ArticleDOI
The Galactic Plane region near ℓ = 93°. II. A stellar wind bubble surrounding SNR 3C 434.1
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Journal ArticleDOI
Forming massive seed black holes in high-redshift quasar host progenitors
TL;DR: In this paper, the conditions for the formation of massive seed BHs from synchronised atomic-cooling halo pairs and/or dynamically heated mini-haloes are investigated in the overdense regions where the progenitors of a typical high-redshift quasar host form and evolve.