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 The Formation of Close Binary Stars

2001 ◽  
Vol 200 ◽  
pp. 23-32 ◽  
Author(s):  
Ian A. Bonnell
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Initial Conditions ◽  
Massive Stars ◽  
Close Binary ◽  
Formation Mechanisms ◽  
Close Binary Systems ◽  
Close Binary Stars ◽  
Orbital Migration

I review the possible formation mechanisms of close binary stars. The formation of close binary systems is problematic in that there is no theory that does not encounter significant difficulties or unknowns. Fission does not appear to occur in stars. Capture is unlikely to form many close binary systems except possibly amongst massive stars. Fragmentation can form close binary systems but these need to accrete the majority of their eventual mass. Furthermore, there appears to be a limited window in initial conditions that may preclude forming sufficient systems in this way. Possible alternatives include the orbital migration of a binary due to its circumbinary disk and the disintegration of a non-hierarchical multiple system.

scholarly journals Interacting Magnetospheres in RS CVn Binaries – Coronal Heating and Flares

1983 ◽  
Vol 71 ◽  
pp. 629-632
Author(s):  
Y. Uchida ◽  
T. Sakurai
Keyword(s):  
Free Energy ◽  
Magnetic Fields ◽  
Binary Systems ◽  
Coronal Heating ◽  
Close Binary ◽  
Magnetic Free Energy ◽  
Close Binary Systems

AbstractCoronae and flares of RS CVn systems are interpreted as due to gradual and sudden releases of magnetic free energy which is built up throught the interaction of magnetic fields of stars in these close binary systems.

scholarly journals Radio Emission from Close Binary Systems and Novae

1977 ◽  
Vol 42 ◽  
pp. 279-291
Author(s):  
R.M. Hjellming
Keyword(s):  
Magnetic Fields ◽  
Radio Emission ◽  
Binary Systems ◽  
Close Binary ◽  
X Ray ◽  
Close Binary Systems ◽  
Nova Shells ◽  
The Subject ◽  
Continuum Radio ◽  
Relativistic Particles

This review of the radio emission properties of close binary systems and novae will be partly concerned with surveying the star systems that exhibit continuum radio emission, and partly concerned with discussing the implications of the observed radio emission. The phenomena we will encounter will range from purely thermal continuum radio emission for the case of ionized nova shells to strong, non-thermal continuum radio emission produced by relativistic particles in both ‘normal’ and X-ray emitting close binary systems. In keeping with the subject of this symposium, let me emphasize that all regions involving radio emission are from the portions of the stellar environment where Ne ≤ 1010cm-3, generally rather high in the stellar or systemic atmosphere; however, events more closely associated with the stars themselves are the root causes of the phenomena, supplying energy, mass, magnetic fields, and relativistic particles.

scholarly journals Candidate Ap stars in close binary systems

2013 ◽  
Vol 9 (S302) ◽  
pp. 313-314 ◽  
Author(s):  
C. P. Folsom ◽  
G. A. Wade ◽  
K. Likuski ◽  
O. Kochukhov ◽  
E. Alecian ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Binary Systems ◽  
Close Binary ◽  
Early Investigation ◽  
Close Binary Systems ◽  
Short Period ◽  
Ap Stars ◽  
Insight Into

AbstractShort period binary systems containing magnetic Ap stars are anomalously rare. This apparent anomaly may provide insight into the origin of the magnetic fields in theses stars. As an early investigation of this, we observed three close binary systems that have been proposed to host Ap stars. Two of these systems (HD 22128 and HD 56495) we find contain Am stars, but not Ap stars. However, for one system (HD 98088) we find the primary is indeed an Ap star, while the secondary is an Am star. Additionally, the Ap star is tidally locked to the secondary, and the predominately dipolar magnetic field of the Ap star is roughly aligned with the secondary. Further investigations of HD 98088 are planned by the BinaMIcS collaboration.

scholarly journals Structure and evolution of massive single stars and their relevance for close binary systems

1995 ◽  
Vol 163 ◽  
pp. 15-23
Author(s):  
Norbert Langer
Keyword(s):  
Binary Systems ◽  
Massive Stars ◽  
Close Binary ◽  
Single Star ◽  
Close Binary Systems ◽  
Massive Close Binary

Differences in the evolution of massive single stars and components of massive close binary systems are investigated. While for stars above the red supergiant luminosity limit, single star and case B primary evolution merge into a single scenario, large differences for less massive stars are demonstrated to occur at the example of MZAMS = 40M⊙, concerning the various WR subtypes, the nucleosynthesis yields, and the supernova stage.

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 The evolution of massive binary systems

2020 ◽  
pp. 1-13
Author(s):  
Jelena Petrovic
Keyword(s):  
Binary Systems ◽  
Gamma Ray ◽  
Massive Stars ◽  
Compact Objects ◽  
Close Binary ◽  
Extensive Literature ◽  
Single Star ◽  
Close Binary Systems ◽  
Massive Binary Systems ◽  
Massive Close Binary

The evolution of massive stars in close binary systems is significantly different from single star evolution due to a series of interactions between the two stellar components. Such massive close binary systems are linked to various astrophysical phenomena, for example Wolf-Rayet stars, supernova type Ib and Ic, X-ray binaries and gamma-ray bursts. Also, the emission of gravitational waves, recently observed by the LIGO-Virgo detectors, is associated with mergers in binary systems containing compact objects, relics of massive stars - black holes and neutron stars. Evolutionary calculations of massive close binary systems were performed by various authors, but many aspects are not yet fully understood. In this paper, the main concepts of massive close binary evolution are reviewed, together with the most important parameters that can influence the final outcome of the binary system evolution, such as rotation, magnetic fields, stellar wind mass loss and mass accretion efficiency during interactions. An extensive literature overview of massive close binary models in the light of exciting observations connected with those systems is presented.

scholarly journals CONSTRAINTS ON THE MASSIVE SUPERNOVA PROGENITORS

2007 ◽  
Vol 16 (07) ◽  
pp. 1219-1228 ◽  
Author(s):  
BOJAN ARBUTINA
Keyword(s):  
Binary Systems ◽  
Massive Stars ◽  
High Redshift ◽  
Practical Importance ◽  
Star Formation History ◽  
Close Binary ◽  
Core Collapse ◽  
B Stars ◽  
Close Binary Systems ◽  
Type Ia

The generally-accepted scheme distinguishes two main classes of supernovae (SNe): Ia resulting from the old stellar population (deflagration of a white dwarf in close binary systems), and SNe of type II and Ib/c whose ancestors are young massive stars (died in a core-collapse explosion). Concerning the latter, there are suggestions that the SNe II are connected to early B stars, and SNe Ib/c to isolated O or Wolf–Rayet (W–R) stars. However, little or no effort was made to further separate SNe Ib from Ic. We have used assumed SN rates for different SN types in spiral galaxies in an attempt to perform this task. If the isolated progenitor hypothesis is correct, our analysis indicates that SNe Ib result from stars of main-sequence mass [Formula: see text], while the progenitors of SNe Ic are more massive stars with [Formula: see text]. Alternatively, if the majority of SNe Ib/c appear in close binary systems (CBs) then they would result from the same progenitor population as most of the SNe II, i.e. early B stars with initial masses of order [Formula: see text]. Future observations of SNe at high-redshift (z) and their rate will provide us with unique information on SN progenitors and the star-formation history of galaxies. At higher-z (deeper in the cosmic past), we expect to see the lack of type Ia events, i.e. the dominance of core-collapse SNe. Better understanding of the stripped-envelope SNe (Ib/c), and their potential use as distance indicators at high-z, would therefore be of great practical importance.

Some Results of the Spectroscopic Study of Four Close Binary Systems of Early Spectral Types

1965 ◽  
Vol 5 ◽  
pp. 120-130
Author(s):  
T. S. Galkina
Keyword(s):  
Spectroscopic Study ◽  
Spectral Type ◽  
Spectroscopic Investigation ◽  
Binary Systems ◽  
Quantitative Information ◽  
Close Binary ◽  
Physical Parameters ◽  
Absorption And Emission ◽  
Close Binary Systems ◽  
Quantitative Estimates

It is necessary to have quantitative estimates of the intensity of lines (both absorption and emission) to obtain the physical parameters of the atmosphere of components.Some years ago at the Crimean observatory we began the spectroscopic investigation of close binary systems of the early spectral type with components WR, Of, O, B to try and obtain more quantitative information from the study of the spectra of the components.

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