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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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2009
This collection of papers from the Space Telescope Science Institute Symposium on massive stars addresses the many aspects of astrophysics in which these stars play an important role. Review papers are presented from both observational and theoretical work by world experts in the study of these rare stars. Topics discussed include star formation in the
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This collection of papers from the Space Telescope Science Institute Symposium on massive stars addresses the many aspects of astrophysics in which these stars play an important role. Review papers are presented from both observational and theoretical work by world experts in the study of these rare stars. Topics discussed include star formation in the
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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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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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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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2004
Supernovae are of wide interest to the astronomical community because they play a key role in the nucleosynthetic evolution of galaxies, stellar remnant populations, the energetics and phase balance of the interstellar medium (ISM), the interpretations of observations of distant galaxies, models of galaxy formation and evolution, the physics of star ...
Patrick A. Young, David Arnett
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Supernovae are of wide interest to the astronomical community because they play a key role in the nucleosynthetic evolution of galaxies, stellar remnant populations, the energetics and phase balance of the interstellar medium (ISM), the interpretations of observations of distant galaxies, models of galaxy formation and evolution, the physics of star ...
Patrick A. Young, David Arnett
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2011
We will define a high-mass star as one with a final mass of greater than 10 M⊙. On the main sequence this group would include stars of spectral type O, B0, and B1. Although stars in this mass range are few in number compared with low-mass stars, they are extremely important with regard to galactic chemical evolution and the physics of the interstellar ...
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We will define a high-mass star as one with a final mass of greater than 10 M⊙. On the main sequence this group would include stars of spectral type O, B0, and B1. Although stars in this mass range are few in number compared with low-mass stars, they are extremely important with regard to galactic chemical evolution and the physics of the interstellar ...
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1999
One of the most durable problems in all of astrophysics is how stars are formed. Since the time of LaPlace astromomers have postulated numerous scenerios, but to the present this problem has resisted solution. This is especially true for massive stars. Massive star formation (MSF) has received much less observational and theoretical attention than low ...
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One of the most durable problems in all of astrophysics is how stars are formed. Since the time of LaPlace astromomers have postulated numerous scenerios, but to the present this problem has resisted solution. This is especially true for massive stars. Massive star formation (MSF) has received much less observational and theoretical attention than low ...
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2007
I.Introduction The formation process of massive O and B stars is arguably the least understood of all stars. The major observational and theoretical emphasis has been concentrated on low mass star formation during the past decade for a varitey of reasons, among which are: it is a more tractable problem than massive star formation and it is well matched
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I.Introduction The formation process of massive O and B stars is arguably the least understood of all stars. The major observational and theoretical emphasis has been concentrated on low mass star formation during the past decade for a varitey of reasons, among which are: it is a more tractable problem than massive star formation and it is well matched
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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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