Showing papers on "Stellar-wind bubble published in 1983"
TL;DR: In this paper, it was shown that stellar winds dominate the energy in the first 4 to 6 million years after which supernovae take over, and a steady-state situation prevails, in which the supernova contribution is dominant.
Abstract: Massive stars (> 20 M⊙) release a considerable amount of mechanical energy in the form of strong stellar winds. A fraction of this energy may be transferred to relativistic cosmic rays by diffusive shock acceleration at the wind boundary, and/or in the expanding, turbulent wind itself. Massive stars are most frequently found in OB associations, surrounded by H ii regions lying at the edge of dense molecular clouds. The interaction of the freshly accelerated particles with matter gives rise to γ-ray emission. In this paper, we first briefly review the current knowledge on the energetics of strong stellar winds from O and Wolf-Rayet stars, as well as from T Tauri stars. Taking into account the finite lifetime of these stars, we then proceed to show that stellar winds dominate the energetics of OB associations during the first 4 to 6 million years, after which supernovae take over. In the solar neighborhood, the star formation rate is constant, and a steady-state situation prevails, in which the supernova contribution is found to be dominant. A small, but meaningful fraction of the COS-B γ-ray sources may be fueled by WR and O stellar winds in OB associations, while the power released by T Tauri stars alone is perhaps insufficient to account for the γ-ray emission of nearby dark clouds. Finally, we discuss some controversial aspects of the physics of particle acceleration by stellar winds.
87 citations
TL;DR: The interaction entre the relativistes of SS 433 and the nebuleuse radio W 50 is analysee sur la base d'observations recentes as mentioned in this paper, and it is probable that SS 433 pourrait etre entouree d'un milieu interstellaire nuageux, du type de celui decrit par le modele a 3 phases de McKee et Ostriker.
Abstract: L'interaction entre les jets relativistes de SS 433 et la nebuleuse radio W 50 est analysee sur la base d'observations recentes. On trouve que SS 433 pourrait etre entouree d'un milieu interstellaire nuageux, du type de celui decrit par le modele a 3 phases de McKee et Ostriker. W 50 est probablement une bulle interstellaire en expansion, entrainee par un fort vent stellaire du compagnon de SS 433 plutot qu'un reste de supernova
28 citations
27 citations
TL;DR: In this article, high-resolution 6 cm observations of two early-type stars have been made with the Very Large Array (VLA) for the first time, showing that Cyg OB2 No 12 appears to have a normal wind with a temperature of about 5000 K; Cyg OO No 9 has unusual radio properties which imply that its radio-emitting circumstellar gas is hotter than 300,000 K.
Abstract: High-resolution 6 cm observations of two early-type stars have been made with the Very Large Array Cyg OB2 No 12 appears to have a normal wind with a temperature of about 5000 K; Cyg OB2 No 9 has unusual and unexpected radio properties which imply that its radio-emitting circumstellar gas is hotter than 300,000 K
26 citations
17 citations
TL;DR: In this article, it was shown that the mass loss rate for the hottest stars, those of 0-type, is proportional to L α, which is predicted by the theory of radiatively driven winds.
15 citations
01 Jan 1983
TL;DR: The most massive stars are losing mass in the form of a more or less steady stellar wind, which blows during most of their lifetime as discussed by the authors, and the energy and momentum of this stellar wind is so large that the wind blows a bubble into the interstellar medium (ISM).
Abstract: The most massive stars are losing mass in the form of a more or less steady stellar wind, which blows during most of their lifetime. The energy and momentum of this stellar wind is so large that the wind blows a bubble into the interstellar medium (ISM). The amount of energy which is deposited into the ISM by the stellar wind during the lifetime of the star is comparable with the energy released in Supernova explosions. In this course I will first review the basic knowledge of the stellar winds (Section II). The theory of the interaction between the wind and the ISM and the structure of a typical interstellar bubble (IB) from a single star is discussed in Section III. A typical example of an observed bubble, the Cygnus Superbubble, is discussed in Section IV.
1 citations