scholarly journals Formation and Evolution of Hypernova Progenitors in Massive Binary Systems

2006 ◽  
pp. 104-112 ◽  
Author(s):  
Paul C. Joss ◽  
J. Alex Becker
Keyword(s):  
Binary Systems ◽  
Massive Binary Systems ◽  
Formation And Evolution

scholarly journals The influence of stellar wind mass loss on the evolution of massive close binaries.

1979 ◽  
Vol 83 ◽  
pp. 409-414
Author(s):  
D. Vanbeveren ◽  
J.P. De Grève ◽  
C. de Loore ◽  
E.L. van Dessel
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Binary Systems ◽  
Mass Loss Rate ◽  
Radiation Force ◽  
Roche Lobe ◽  
Close Binaries ◽  
Massive Binary Systems ◽  
Binary Evolution ◽  
X Ray Binaries

It is generally accepted that massive (and thus luminous) stars lose mass by stellar wind, driven by radiation force (Lucy and Solomon, 1970; Castor et al. 1975). For the components of massive binary systems, rotational and gravitational effects may act together with the radiation force so as to increase the mass loss rate. Our intention here is to discuss the influence of a stellar wind mass loss on the evolution of massive close binaries. During the Roche lobe overflow phase, mass and angular momentum can leave the system. Possible reasons for mass loss from the system are for example the expansion of the companion due to accretion of the material lost by the mass losing star (Kippenhahn and Meyer-Hofmeister, 1977) or the fact that due to the influence of the radiation force in luminous stars, mass will be lost over the whole surface of the star and not any longer through a possible Lagrangian point as in the case of classical Roche lobe overflow (Vanbeveren, 1978). We have therefore investigated the influence of both processes on binary evolution. Our results are applied to 5 massive X-ray binaries with a possible implication for the existence of massive Wolf Rayet stars with a very close invisible compact companion. A more extended version of this talk is published in Astronomy and Astrophysics (Vanbeveren et al. 1978; Vanbeveren and De Grève, 1978). Their results will be briefly reviewed.

scholarly journals Hunting for Dwarf Galaxies Hosting the Formation and Coalescence of Compact Binaries

Physics ◽  
2019 ◽  
Vol 1 (3) ◽  
pp. 412-429 ◽  
Author(s):  
Luca Graziani
Keyword(s):  
Binary Systems ◽  
Local Group ◽  
Dwarf Galaxies ◽  
Large Population ◽  
Compact Binaries ◽  
Compact Binary ◽  
The Galaxy ◽  
Low Metallicity ◽  
Formation And Evolution ◽  
Galaxy Assembly

Here we introduce the latest version of the GAMESH model, capable to consistently account for the formation and evolution of compact binary systems along the cosmic assembly of a Milky Way (MW)-like galaxy, centered on a local group volume resolving a large population of dwarf satellites. After describing the galaxy assembly process and how the formation of binary systems is accounted for, we summarize some recent findings on the properties and evolution of low-metallicity dwarf galaxies hosting the birth/coalescence of stellar/compact binaries generating GW150914-like signals. Finally, we focus on the mass and orbital properties of the above compact binary candidates assessing their impact on the resulting coalescence times and on selecting suitable galaxy hosts.

scholarly journals The formation and evolution of binary systems

2001 ◽  
Vol 375 (3) ◽  
pp. 989-998 ◽  
Author(s):  
J. Bouvier ◽  
G. Duchêne ◽  
J.-C. Mermilliod ◽  
T. Simon
Keyword(s):  
Binary Systems ◽  
Formation And Evolution

scholarly journals Line-Profile Variations on Massive Binary Systems: Determining η Carinae Orbital Parameters

2006 ◽  
Vol 2 (S240) ◽  
pp. 198-201
Author(s):  
D. Falceta-Gonçalves ◽  
Z. Abraham ◽  
V. Jatenco-Pereira
Keyword(s):  
Line Profile ◽  
Binary Systems ◽  
Spectral Lines ◽  
Stream Velocity ◽  
Interaction Zone ◽  
Orbital Inclination ◽  
Orbital Parameters ◽  
Massive Binary Systems ◽  
Shock Fronts ◽  
Synthetic Line

AbstractWhen the winds of two massive stars orbiting each other collide, an interaction zone is created consisting of two shock fronts at both sides of a contact surface. During the cooling process, elements may recombine generating spectral lines. These lines may be Doppler shifted, as the gas stream flows over the interaction zone. To calculate the stream velocity projected into the line of sight we use a simplified conical geometry for the shock fronts and, to determine the synthetic line profile, we have to sum the amount of emitting gas elements with the same Doppler shifted velocity. We show that the stellar mass loss rates and wind velocities, and the orbital inclination and eccentricity, are the main parameters on this physical process. By comparing observational data to the synthetic line profiles it is possible to determine these parameters. We tested this process to Brey 22 WR binary system, and applied to the enigmatic object of η Carinae.

scholarly journals Is there a Connection Between Non-Synchronous Rotation and X-Ray Emission in Massive Binary Systems?

2004 ◽  
Vol 215 ◽  
pp. 163-165 ◽  
Author(s):  
Sinhué Haro ◽  
Juan Antonio Juárez ◽  
Gloria Koenigsberger
Keyword(s):  
Mass Loss ◽  
Orbital Period ◽  
Binary Systems ◽  
X Ray ◽  
Rotating Systems ◽  
Tidal Forces ◽  
Synchronous Rotation ◽  
Massive Binary Systems ◽  
Loss Rates

A correlation between orbital period and log(LX/Lbol) is found for a sample of B-type binary systems. We suggest that wind-wind collisions are the likely mechanism for generating the X-ray emission, and that the mass-loss rates may be enhanced in non-synchronously rotating systems due to the oscillations that are excited by the tidal forces.

scholarly journals Shaping bipolar and elliptical Planetary Nebulae: Rotation and magnetic field

1997 ◽  
Vol 180 ◽  
pp. 226-226 ◽  
Author(s):  
Guillermo García-Segura ◽  
Norbert Langer ◽  
Michał Różyczka ◽  
Mordechai-Mark Mac Low ◽  
José Franco
Keyword(s):  
Magnetic Field ◽  
Ionizing Radiation ◽  
Radiation Field ◽  
Binary Systems ◽  
Planetary Nebulae ◽  
Stellar Rotation ◽  
Central Source ◽  
Formation And Evolution

We present hydrodynamical and magnetohydronynamical simulations for the formation and evolution of bipolar and elliptical planetary nebulae with two interacting winds. The models are performed under the hypothesis of a single central source, i.e. binary systems are not considered and a single initial wind function is used in our calculations. We explore various relevant parameters, including the effects of stellar rotation, ionizing radiation field and stellar magnetic field, and a catalogue of resulting shapes is generated.

scholarly journals Massive runaway and walkaway stars

2019 ◽  
Vol 624 ◽  
pp. A66 ◽  
Author(s):  
M. Renzo ◽  
E. Zapartas ◽  
S. E. de Mink ◽  
Y. Götberg ◽  
S. Justham ◽  
...  
Keyword(s):  
Binary Systems ◽  
Numerical Study ◽  
Core Collapse ◽  
Mass Distributions ◽  
Peculiar Velocities ◽  
Order Of Magnitude ◽  
Massive Binary Systems ◽  
Stringent Test ◽  
Binary Evolution ◽  
Runaway Stars

We perform an extensive numerical study of the evolution of massive binary systems to predict the peculiar velocities that stars obtain when their companion collapses and disrupts the system. Our aim is to (i) identify which predictions are robust against model uncertainties and assess their implications, (ii) investigate which physical processes leave a clear imprint and may therefore be constrained observationally, and (iii) provide a suite of publicly available model predictions to allow for the use of kinematic constraints from the Gaia mission. We find that 22+26−8% of all massive binary systems merge prior to the first core-collapse in the system. Of the remainder, 86+11−9% become unbound because of the core-collapse. Remarkably, this rarely produces runaway stars (observationally defined as stars with velocities above 30 km s−1). These are outnumbered by more than an order of magnitude by slower unbound companions, or “walkaway stars”. This is a robust outcome of our simulations and is due to the reversal of the mass ratio prior to the explosion and widening of the orbit, as we show analytically and numerically. For stars more massive than 15 M⊙, we estimate that 10+5−8% are walkaways and only 0.5+1.0−0.4% are runaways, nearly all of which have accreted mass from their companion. Our findings are consistent with earlier studies; however, the low runaway fraction we find is in tension with observed fractions of about 10%. Thus, astrometric data on presently single massive stars can potentially constrain the physics of massive binary evolution. Finally, we show that the high end of the mass distributions of runaway stars is very sensitive to the assumed black hole natal kicks, and we propose this as a potentially stringent test for the explosion mechanism. We also discuss companions remaining bound that can evolve into X-ray and gravitational wave sources.

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