Pre-supernova Evolution and Nucleosynthesis in Massive Stars and Their Stellar Wind Contribution

2017 ◽  
pp. 1-51
Author(s):  
Raphael Hirschi
Keyword(s):  
Stellar Wind ◽  
Massive Stars

scholarly journals Enrichment by Wolf-Rayet Stars and Other Massive Stars in Gas, Dust and Energy

1991 ◽  
Vol 143 ◽  
pp. 323-334
Author(s):  
Martin Cohen
Keyword(s):  
Interstellar Medium ◽  
Infrared Spectra ◽  
Stellar Wind ◽  
Massive Stars ◽  
Observational Evidence ◽  
Radiative Energy ◽  
New Members ◽  
Hot Gas ◽  
Sn 1987A ◽  
Dust Mass

I update previous estimates of the separate contributions for radiative energy, integrated total stellar wind mass and dust mass from Wolf-Rayet stars and other massive (OBA) stars. In the context of the intriguing dusty WC9 stars, I: (1) discuss the observability (or otherwise) between 0.4 and 23 μm of the condensation route from hot gas to carbon-rich grains; (2) urge caution in the use of 10 μm infrared spectra of these luminous stars to deduce the importance of silicates as a component of the interstellar medium, and (3) speculate on a possible new method for discovering new members of this relatively rare subtype based on IRAS Low Resolution Spectra. I review the observational evidence for dust condensation around SN 1987A.

scholarly journals On the significance of mass loss for the evolution of massive stars

1981 ◽  
Vol 59 ◽  
pp. 265-270
Author(s):  
L.R. Yungelson ◽  
A.G. Massevitch ◽  
A.V. Tutukov
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Loss Rate ◽  
Massive Stars ◽  
Mass Loss Rate ◽  
Hydrogen Burning ◽  
B Stars ◽  
The Core ◽  
Input Parameters ◽  
Satisfactory Theory

It is shown that mass loss by stellar wind with rates observed in O, B-stars cannot change qualitatively their evolution in the core hydrogen-burning stage. The effects, that are usually attributed to the mass loss, can be explained by other causes: e.g., duplicity or enlarged chemically homogeneous stellar cores.The significance of mass loss by stellar wind for the evolution of massive stars was studied extensively by numerous authors (see e.g. Chiosi et al. (1979) and references therein). However, the problem is unclear as yet. There does not exist any satisfactory theory of mass loss by stars. Therefore one is usually forced to assume that mass loss rate depends on some input parameters.

scholarly journals The B[e] stars

1989 ◽  
Vol 113 ◽  
pp. 117-120
Author(s):  
F.-J. Zickgraf
Keyword(s):  
Physical Properties ◽  
Stellar Wind ◽  
Main Sequence ◽  
Massive Stars ◽  
High Mass ◽  
Sequence Evolution ◽  
Two Component ◽  
Show Evidence ◽  
High Mass Loss ◽  
General Appearance

AbstractB[e] supergiants show evidence for a non-spherical two-component stellar wind. The general appearance and the physical properties of the suggested disk-like configuration are discussed. The high mass-loss rates, the surprisingly large number and the location in the H-R diagram make these stars important for the understanding of the post-main-sequence evolution of massive stars.

scholarly journals Some observations relevant to the theory of extended envelopes

1987 ◽  
Vol 122 ◽  
pp. 409-423
Author(s):  
B. Wolf
Keyword(s):  
Emission Line ◽  
Stellar Wind ◽  
Massive Stars ◽  
Spatially Resolved ◽  
The Universe

Recent observations of S Dor variables and B[e]-supergiants are reviewed. These objects belong to the visually and bolometrically brightest stars in the universe. They have gained considerable interest for their exceptional stellar wind properties and represent rare cases of hot blue stars which form dust envelopes. S Dor variables are characterized by major outbursts. The ejecta have been spatially resolved in some cases. These luminous emission line stars are supposed to represent a short-lived phase in the evolution of the very massive stars prior to becoming WR stars.

Mass Loss and Stellar Wind in Massive X-Ray Binaries

1980 ◽  
Vol 5 ◽  
pp. 541-547
Author(s):  
H. F. Henrichs
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Binary Systems ◽  
Massive Stars ◽  
Compact Star ◽  
X Rays ◽  
Early Type ◽  
X Ray ◽  
X Ray Binaries ◽  
Loss Rates

A number of massive stars of early type is found in X-ray binary systems. The catalog of Bradt et al. (1979) contains 21 sources optically identified with massive stars ranging in spectral type from 06 to B5 out of which 13 are (nearly) unevolved stars and 8 are supergiants. Single stars of this type generally show moderate to strong stellar winds. The X-rays in these binaries originate from accretion onto a compact companion (we restrict the discussion to this type of X-rays).We consider the compact star as a probe traveling through the stellar wind. This probe enables us to derive useful information about the mass outflow of massive stars.After presenting the basic data we derive an upper limit to mass loss rates of unevolved early type stars by studying X-ray pulsars. Next we consider theoretical predictions concerning the influence of X-rays on the stellar wind and compare these with the observations. Finally, using new data from IUE, we draw some conclusions about mass loss rates and velocity laws as derived from X-ray binaries.

scholarly journals Ultraviolet spectra of extreme nearby star-forming regions: Evidence for an overabundance of very massive stars

2021 ◽  
Vol 503 (4) ◽  
pp. 6112-6135
Author(s):  
Peter Senchyna ◽  
Daniel P Stark ◽  
Stéphane Charlot ◽  
Jacopo Chevallard ◽  
Gustavo Bruzual ◽  
...  
Keyword(s):  
Stellar Wind ◽  
Massive Stars ◽  
Stellar Populations ◽  
Population Synthesis ◽  
Nearby Star ◽  
Star Forming ◽  
Star Forming Regions ◽  
High Incidence ◽  
Stellar Population Synthesis ◽  
Stellar Masses

ABSTRACT As deep spectroscopic campaigns extend to higher redshifts and lower stellar masses, the interpretation of galaxy spectra depends increasingly upon models for very young stellar populations. Here we present new HST/COS ultraviolet spectroscopy of seven nearby (<120 Mpc) star-forming regions hosting very young stellar populations (∼4–20 Myr) with optical Wolf–Rayet stellar wind signatures, ideal laboratories in which to benchmark these stellar models. We detect nebular C iii] in all seven, but at equivalent widths uniformly <10 Å. This suggests that even for very young stellar populations, the highest equivalent width C iii] emission at ≥15 Å is reserved for inefficiently cooled gas at metallicities at or below that of the SMC. The spectra also reveal strong C iv P-Cygni profiles and broad He ii emission formed in the winds of massive stars, including some of the most prominent He ii stellar wind lines ever detected in integrated spectra. We find that the latest stellar population synthesis prescriptions with improved treatment of massive stars nearly reproduce the entire range of stellar He ii wind strengths observed here. However, we find that these models cannot simultaneously match the strongest wind features alongside the optical nebular line constraints. This discrepancy can be naturally explained by an overabundance of very massive stars produced by a high incidence of binary mass transfer and mergers occurring on short ≲10 Myr time-scales, suggesting these processes may be crucial for understanding systems dominated by young stars both nearby and in the early Universe.

scholarly journals How to inflate a wind-blown bubble

2021 ◽  
Vol 508 (2) ◽  
pp. 1768-1776
Author(s):  
J M Pittard ◽  
C J Wareing ◽  
M M Kupilas
Keyword(s):  
Stellar Wind ◽  
External Medium ◽  
Reference Model ◽  
Massive Stars ◽  
Ambient Medium ◽  
Stellar Winds ◽  
Relative Importance ◽  
Numerical Resolution ◽  
Maximum Value ◽  
Injection Region

ABSTRACT Stellar winds are one of several ways that massive stars can affect the star formation process on local and galactic scales. In this paper, we investigate the numerical resolution needed to inflate an energy-driven stellar wind bubble in an external medium. We find that the radius of the wind injection region, rinj, must be below a maximum value, rinj,max, in order for a bubble to be produced, but must be significantly below this value if the bubble properties are to closely agree with analytical predictions. The final bubble momentum is within 25 per cent of the value from a higher resolution reference model if χ = rinj/rinj,max = 0.1. Our work has significance for the amount of radial momentum that a wind-blown bubble can impart to the ambient medium in simulations, and thus on the relative importance of stellar wind feedback.

scholarly journals Is Stellar Wind Mass Loss During Core Hydrogen Burning Important for Evolution

1991 ◽  
Vol 143 ◽  
pp. 547-547
Author(s):  
R. Blomme ◽  
D. Vanbeveren ◽  
W. Van Rensbergen
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Massive Stars ◽  
Hydrogen Burning

The influence of wind mass loss during core hydrogen burning on the evolution of massive stars can be investigated using a relation between Ṁ-L-M-Teff based on

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