scholarly journals Massive binaries as progenitors for stellar explosions

2015 ◽  
Vol 11 (A29B) ◽  
pp. 208-208
Author(s):  
Selma de Mink
Keyword(s):  
Strong Interaction ◽  
Orbital Period ◽  
Binary Systems ◽  
Massive Stars ◽  
Binary Star ◽  
Close Binary ◽  
Population Synthesis ◽  
Close Binary Systems ◽  
Star Models ◽  
The Masses

AbstractThe majority of young massive stars are found in close binary systems. Recently, dedicated observingcampaigns have provided strong constraints on the binary fraction as well as the distribution of the parameters thatcharacterize the binary systems: the masses of both components, the orbital period and eccentricities. Most strikinglythese findings imply that the majority of massive stars experience strong interaction (roche lobe overflow, a commonenvelope phase and or a merger) with a binary companion before their final explosion. I will discuss recent resultsfrom detailed binary star models and population synthesis models.

scholarly journals Formation of cold clumps and filaments around superbubbles

2015 ◽  
Vol 11 (A29B) ◽  
pp. 231-231
Author(s):  
E. Ntormousi ◽  
P. Hennebelle ◽  
J. Dawson ◽  
F. Del Sordo
Keyword(s):  
Strong Interaction ◽  
Orbital Period ◽  
Binary Systems ◽  
Massive Stars ◽  
Binary Star ◽  
Close Binary ◽  
Population Synthesis ◽  
Common Envelope ◽  
Star Models ◽  
The Masses

AbstractThe majority of young massive stars are found in close binary systems. Recently, dedicated observing campaigns have provided strong constraints on the binary fraction as well as the distribution of the parameters that characterize the binary systems: the masses of both components, the orbital period and eccentricities. Most strikingly these findings imply that the majority of massive stars experience strong interaction (roche lobe overflow, a common envelope phase and or a merger) with a binary companion before their final explosion. I will discuss recent results from detailed binary star models and population synthesis models.

scholarly journals HD 50896: an other WR binary star

1979 ◽  
Vol 83 ◽  
pp. 421-424
Author(s):  
C. Firmani ◽  
G. Koenigsberger ◽  
G. F. Bisiacchi ◽  
E. Ruíz ◽  
A. Solar
Keyword(s):  
Large Distance ◽  
Binary Systems ◽  
Galactic Plane ◽  
Binary Star ◽  
Close Binary ◽  
Average Height ◽  
Close Binary Systems ◽  
First Time

The current ideas concerning the evolution of close binary systems (van den Heuvel, 1976), accepting the hypothesis that the system is not disrupted by the first supernova (SN) explosion, predict that the Wolf-Rayet phase can occur twice. The first time the companion of the WR star is a normal OB star and the second time it is a collapsed object. In this context, the importance of searching for binary systems with collapsed companions among the “single” WR stars is evident. Due to its large distance from the galactic plane, z = 280 pc (Smith, 1968a), when compared with the average height (z = 60 pc, Cruz-González et al., 1974) of extreme Population I stars, HD 50896 was considered to be a likely candidate to this type of system.

scholarly journals Superoutbursts and Superhumps of SU UMa Stars

1988 ◽  
Vol 108 ◽  
pp. 238-239
Author(s):  
Yoji Osaki ◽  
Masahito Hirose
Keyword(s):  
Accretion Disk ◽  
Orbital Period ◽  
White Dwarf ◽  
Binary Systems ◽  
Roche Lobe ◽  
Light Curves ◽  
Close Binary ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Close Binary Systems

SU UMa stars are one of subclasses of dwarf novae. Dwarf novae are semi-detached close binary systems in which a Roche-lobe filling red dwarf secondary loses matter and the white dwarf primary accretes it through the accretion disk. The main characteristics of SU UMa subclass is that they show two kinds of outbursts: normal outbursts and superoutbursts. In addition to the more frequent narrow outbursts of normal dwarf nova, SU UMa stars exhibit “superoutbursts”, in which stars reach about 1 magnitude brighter and stay longer than in normal outburst. Careful photometric studies during superoutburst have almost always revealed the “superhumps”: periodic humps in light curves with a period very close to the orbital period of the system. However, the most curious of all is that this superhump period is not exactly equal to the orbital period, but it is always longer by a few percent than the orbital period.

scholarly journals Internal magnetic fields, spin-orbit coupling, and orbital period modulation in close binary systems

2019 ◽  
Author(s):  
A F Lanza
Keyword(s):  
Orbital Period ◽  
Binary Systems ◽  
Orbit Coupling ◽  
Close Binary ◽  
Spin Orbit Coupling ◽  
Spin Orbit ◽  
Active Components ◽  
Momentum Exchange ◽  
Hot Jupiters ◽  
Close Binary Systems

Abstract We introduce a new model to explain the modulation of the orbital period observed in close stellar binary systems based on an angular momentum exchange between the spin of the active component and the orbital motion. This spin-orbit coupling is not due to tides, but is produced by a non-axisymmetric component of the gravitational quadrupole moment of the active star due to a persistent non-axisymmetric internal magnetic field. The proposed mechanism easily satisfies all the energy constraints having an energy budget ∼102 − 103 times smaller than those of previously proposed models and is supported by the observations of persistent active longitudes in the active components of close binary systems. We present preliminary applications to three well-studied binary systems to illustrate the model. The case of stars with hot Jupiters is also discussed showing that no significant orbital period modulation is generally expected on the basis of the proposed model.

scholarly journals On the Masses of the White Dwarfs in Classical Nova Systems

1989 ◽  
Vol 114 ◽  
pp. 498-506 ◽  
Author(s):  
James W. Truran ◽  
Mario Livio
Keyword(s):  
White Dwarf ◽  
Binary Systems ◽  
Close Binary ◽  
Critical Parameters ◽  
Significant Progress ◽  
Classical Novae ◽  
The Past ◽  
Close Binary Systems ◽  
Classical Nova ◽  
The Masses

Significant progress in our understanding of the nature of the outbursts of the classical novae has occurred over the past two decades (see, e.g., reviews by Truran 1982; Starrfield 1986). Their outbursts are now understood to be driven by thermonuclear runaways proceeding in the accreted hydrogen-rich shells on the white dwarf components of close binary systems. Critical parameters which serve to dictate the varied characteristics of the observed outbursts include the intrinsic white dwarf luminosity, the rate of mass accretion, the composition of the envelope matter prior to runaway, and the white dwarf mass.

scholarly journals The BinaMIcS project: understanding the origin of magnetic fields in massive stars through close binary systems

2014 ◽  
Vol 9 (S307) ◽  
pp. 330-335 ◽  
Author(s):  
E. Alecian ◽  
C. Neiner ◽  
G. A. Wade ◽  
S. Mathis ◽  
D. Bohlender ◽  
...  
Keyword(s):  
Magnetic Properties ◽  
Magnetic Fields ◽  
Binary Systems ◽  
Initial Conditions ◽  
Massive Stars ◽  
Close Binary ◽  
First Year ◽  
Close Binary Systems ◽  
Stellar Formation ◽  
Formation And Evolution

AbstractIt is now well established that a fraction of the massive (M> 8M⊙) star population hosts strong, organised magnetic fields, most likely of fossil origin. The details of the generation and evolution of these fields are still poorly understood. The BinaMIcS project takes an important step towards the understanding of the interplay between binarity and magnetism during the stellar formation and evolution, and in particular the genesis of fossil fields, by studying the magnetic properties of close binary systems. The components of such systems are most likely formed together, at the same time and in the same environment, and can therefore help us to disentangle the role of initial conditions on the magnetic properties of the massive stars from other competing effects such as age or rotation. We present here the main scientific objectives of the BinaMIcS project, as well as preliminary results from the first year of observations from the associated ESPaDOnS and Narval spectropolarimetric surveys.

scholarly journals Rotation and Massive Close Binary Evolution

2007 ◽  
Vol 3 (S250) ◽  
pp. 167-178 ◽  
Author(s):  
Norbert Langer ◽  
Matteo Cantiello ◽  
Sung-Chul Yoon ◽  
Ian Hunter ◽  
Ines Brott ◽  
...  
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Single Star ◽  
Essential Ingredient ◽  
Critical Rotation ◽  
Close Binary Systems ◽  
Star Models ◽  
Binary Evolution ◽  
Massive Close Binary

AbstractWe review the role of rotation in massive close binary systems. Rotation has been advocated as an essential ingredient in massive single star models. However, rotation clearly is most important in massive binaries where one star accretes matter from a close companion, as the resulting spin-up drives the accretor towards critical rotation. Here, we explore our understanding of this process, and its observable consequences. When accounting for these consequences, the question remains whether rotational effects in massive single stars are still needed to explain the observations.

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