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The Formation of Stars
Our galaxy is composed of billions of stars concentrated in the galactic plane, surrounded by interstellar gas, which is mainly composed of hydrogen. About half of the hydrogen is distributedExpand
Spin-up and hot spots can drive mass out of a binary
Context. The observed distribution of orbital periods of Algols with a B-type primary at birth agrees fairly well with the prediction from conservative theory. Conservative evolution fails, however,Expand
The WR and O-type star population predicted by massive star evolutionary synthesis
Abstract Evolutionary calculations of massive single stars and of massive close binaries that we use in the population number synthesis (PNS) code are presented. Special attention is given to theExpand
The Brightest Binaries
Constants massive stars massive single stars massive close binaries massive star population number synthesis.
Simultaneous ultraviolet, optical, and X-ray observations of the X-ray source Vela X-1 /HD 77581/
Ultraviolet spectra of HD 77581, associated with the binary X-ray source Vela X-1, taken with the International Ultraviolet Explorer satellite (IUE) show a spectrum typical of an early B-typeExpand
Mass loss out of close binaries. The formation of Algol-type systems, completed with case B RLOF
Context. Several authors have previously introduced liberal evolution of interacting binaries, with the purpose of meeting various observed binary characteristics better than with conservativeExpand
Nucleosynthesis and evolution of massive stars with mass loss and overshooting
The evolution of mass-losing stars that have M(ZAMS)/solar-M in the 50-100 range is examined. The stellar models used in this study include: (1) mass loss formalism for O, Of, and W-R stars; (2) theExpand
Mass loss out of close binaries. II
Liberal evolution of interacting binaries has been proposed previously by several authors in order to meet various observed binary characteristics better than conservative evolution does. SinceExpand
Structure and evolution of single and binary stars
Foreword. 1. Introduction to the Stars. 2. The Equations of Stellar Structure. 3. The Equation of State. 4. Nuclear Reaction Rates. 5. Nuclear Burning in Stellar Interiors. 6. AstrophysicalExpand
Mass loss from alpha Cyg /A2Ia/ derived from the profiles of low excitation Fe II lines
The low-excitation Fe II lines in the spectral region 2000-3000 A are studied in the spectrum of alpha-Cyg. The profiles of the resonance lines are described by four representative parameters, and aExpand
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