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The Formation of Massive Stars
Astronomische Nachrichten, 2004B 01 A Massive Accretion Disk in M17 B 02 A VLT/ISAAC Study of the Cluster in M17 B 03 Multi-line Observations of the ON-1 Molecular Cloud/H II Region B 04 VLA 7 mm Observations Toward the Pumping Heart of GGD27 B 05 Stellar Masers in Massive Star Forming Regions B 06 The Decay of Massive Cores of Young Star Clusters
Nielbock, Markus +5 more
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The drivers of massive star evolution
Science, 2023An elusive population of stripped binary stars is finally ...
Jon, Sundqvist, Hugues, Sana
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Nucleosynthesis in Massive Stars
Space Science Reviews, 1993We discuss three aspects of the nucleosynthesis in massive and intermediate—mass stars during their early evolutionary phases. These are related to the CNO abundances in giant or supergiant stars, to the 26A1 yield from massive stars via stellar wind, and to the production of the s—process nuclei in massive stars.
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The Evolution of Massive Binary Stars
Annual Review of Astronomy and AstrophysicsMassive stars play a major role in the evolution of their host galaxies and serve as important probes of the distant Universe. It has been established that the majority of massive stars reside in close binaries and interact with their companion stars during their lifetimes.
P Marchant, J Bodensteiner
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The evolution of massive stars to explosion
Space Science Reviews, 1994We review the possible evolutionary paths from massive stars to explosive endpoints as various types of supernovae associated with Population I and hence with massive stars: Type II-P, Type II-L, Type Ib, Type Ic, and the hybrid events SN 1987K and SN 1993J.
J. C. Wheeler, D. A. Swartz
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1989
The term massive star is not very precise, and in the following we shall use it for stars with zero age main sequence (ZAMS) masses M ZAMS above approximately 15 M ⊙. Note, however, that these abjects may achieve actual masses well below 15 M ⊙ during their evolution, as a consequence of mass loss due to stellar winds, pulsations, or other processes. M
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The term massive star is not very precise, and in the following we shall use it for stars with zero age main sequence (ZAMS) masses M ZAMS above approximately 15 M ⊙. Note, however, that these abjects may achieve actual masses well below 15 M ⊙ during their evolution, as a consequence of mass loss due to stellar winds, pulsations, or other processes. M
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Massive Stars: Setting the Stage
Space Science Reviews, 1993The paper gives a summary of the situation mid-1993 of theory and observations regarding massive stars. I describe: stellar mass loss and its implications, pre-main-sequence evolution, the main sequence, problems of atmospheric instability, Luminous Blue Supergiants, Yellow Hyper-giants, Wolf—Rayet stars and supernovae.
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Wind asymmetries in massive stars
Space Science Reviews, 1994We are in the process of surveying the linear polarization in luminous, early-type stars. We here report on new observations of the B [e] stars S 18 and R 50, and of the Luminous Blue Variables HR Car, R 143, and HD 160529. Together with previously published data, these observations provide clear evidence for the presence of intrinsic polarization in 1
R. E. Schulte-Ladbeck +6 more
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Massive stars in the galactic center
New Astronomy Reviews, 2000We review quantitative spectroscopic studies of massive stars in the Galactic Center clusters. Thanks to the impressive evolution of IR detectors an the new generation of line blanketed models for the extended atmospheres of hot stars we are able to accurately derive the physical properties of the massive stars in these clusters.
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