scholarly journals Rapid binary star evolution for N-body simulations and population synthesis

1997 ◽  
Vol 291 (4) ◽  
pp. 732-748 ◽  
Author(s):  
C. A. Tout ◽  
S. J. Aarseth ◽  
O. R. Pols ◽  
P. P. Eggleton
Keyword(s):  
Binary Star ◽  
Population Synthesis ◽  
Star Evolution

scholarly journals Extreme Horizontal Branch Stars in Passively Evolving Early Type Galaxies

2012 ◽  
Vol 10 (H16) ◽  
pp. 120-120
Author(s):  
Fabiola Hernández-Pérez ◽  
Gustavo Bruzual
Keyword(s):  
Binary Star ◽  
Horizontal Branch ◽  
Population Synthesis ◽  
Early Type ◽  
Star Evolution ◽  
Horizontal Branch Stars ◽  
Uv Excess ◽  
Ehb Stars

AbstractWe study the effects of including binary star evolution in population synthesis models. We use the Hurley et al. (2002) code to compute binary star evolutionary tracks, and follow the procedure by Han et al. (2002), in particular, the two 2HeWD merger channel, to form EHB stars from a binary pair. We apply the resulting models to study UV excess ETGs.

scholarly journals Neutron star masses

2012 ◽  
Vol 8 (S291) ◽  
pp. 146-146
Author(s):  
David Nice
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Observational Data ◽  
Mass Distribution ◽  
Binary Star ◽  
Star Mass ◽  
Star Evolution ◽  
Neutron Star Mass ◽  
Present Understanding

AbstractNeutron star masses can be inferred from observations of binary pulsar systems, particularly by the measurement of relativistic phenomena within these orbits. The observed distribution of masses can be used to infer or constrain the equation of state for nuclear matter and to study astrophysical processes such as supernovae and binary star evolution. In this talk, I will review our present understanding of the neutron star mass distribution with an emphasis on the observational data.

scholarly journals The symbiotics as binary stars

1982 ◽  
Vol 70 ◽  
pp. 231-251
Author(s):  
Mirek J. Plavec
Keyword(s):  
Mass Transfer ◽  
Binary Stars ◽  
Binary Star ◽  
Evolutionary Stage ◽  
Cool Component ◽  
Second Stage ◽  
Star Evolution ◽  
Red Giant ◽  
Helium Star ◽  
Central Stars

AbstractSymbiotic stars have become an important testing ground of various theories of binary star evolution. Several physically different models can explain them, but in each case certain fairly restrictive conditions must be met, so if we manage to identify a definite object with a model, it will tell us a lot about the structure and evolutionary stage of the stars involved. I envisage at least three models that can give us a symbiotic object: I have called them, respectively, the PN symbiotic, the Algol symbiotic, and the novalike symbiotic. Their properties are briefly discussed. The most promising model is one of a binary system in the second stage of mass transfer, actually at the beginning of it: The cool component is a red giant ascending the asymptotic branch, expanding but not yet filling its critical lobe. The hot star is a subdwarf located in the same region of the Hertzsprung-Russell diagram as the central stars of planetary nebulae. It may be closely related to them, or it may be a helium star, actually a remnant of an Algol primary which underwent the first stage of mass transfer. In these cases, accretion on this star may not play a significant role (PN symbiotic).

scholarly journals The interstellar medium around Wolf-Rayet stars: clues to evolution

1995 ◽  
Vol 163 ◽  
pp. 34-42
Author(s):  
Joy S. Nichols
Keyword(s):  
Supernova Remnants ◽  
Binary Systems ◽  
Binary Star ◽  
Theoretical Models ◽  
Current Data ◽  
Optical Data ◽  
Photometric Variability ◽  
Star Evolution ◽  
Ring Nebula ◽  
Multi Wavelength

Multi-wavelength investigations of the interstellar environment around WR stars using IUE, IRAS, and optical data have led to the discovery of extended shells of gas and dust 50-100 pc in diameter in the lines of sight to the WR stars HD 50896, HD 96548, and HD 192163. These three stars share several common characteristics: (1) associated N- and He-enriched ring nebula, (2) spectral class WN5-8, and (3) spectral and photometric variability. Surveys of IUE spectra and IRAS images reveal a few additional candidates for such extended shells. Although positional coincidences cannot be excluded, possible origins of these extended shells include interstellar bubbles formed by stellar winds, non-conservative mass loss from binary systems, and supernova remnants. Current data suggest these three stars may be in a post X-ray binary stage, representing the second WR phase of massive binary star evolution. The discovery of extended shells of gas and dust possibly related to WR stars is important because the search for stars in the second WR phase, after the supernova of the primary, has been quite elusive. However, the observational evidence and available theoretical models for post-supernova massive binary star evolution and subsequent non-conservative mass transfer are not yet sufficient to firmly identify the origins of these extended shells.

Type Ib/Ic/IIb/II-L Supernovae and Binary Star Evolution

1995 ◽  
Vol 759 (1) ◽  
pp. 360-367 ◽  
Author(s):  
K. NOMOTO ◽  
K. IWAMOTO ◽  
H. YAMAOKA ◽  
T. SUZUKI ◽  
O.R. POLS ◽  
...  
Keyword(s):  
Binary Star ◽  
Star Evolution

MASS-TRANSFER EFFECTS IN BINARY STAR EVOLUTION

1977 ◽  
Vol 302 (1 Eighth Texas) ◽  
pp. 36-46 ◽  
Author(s):  
Brian P. Flannery
Keyword(s):  
Mass Transfer ◽  
Binary Star ◽  
Transfer Effects ◽  
Star Evolution

scholarly journals Global characteristics of the first IBIS/ISGRI catalogue sources: unveiling a murky episode of binary star evolution

2005 ◽  
Vol 443 (2) ◽  
pp. 485-494 ◽  
Author(s):  
A. J. Dean ◽  
A. Bazzano ◽  
A. B. Hill ◽  
J. B. Stephen ◽  
L. Bassani ◽  
...  
Keyword(s):  
Binary Star ◽  
Star Evolution
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