scholarly journals Binary Stars: Historical Milestones

2001 ◽  
Vol 200 ◽  
pp. 1-12 ◽  
Author(s):  
Hans Zinnecker
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Binary Star ◽  
Historical Review ◽  
History Of Ideas ◽  
Double Stars ◽  
Spectroscopic Binary ◽  
History Of ◽  
Statistical Argument ◽  
Definition Of

This is a brief historical review of the discovery of binary stars, starting in the 18th and 19th century with the work of W. Herschel, W. Struve, and their famous sons. I describe how Ch. Doppler in 1842 found the Doppler effect in connection with the colours of double stars. I also describe how the observation of the stationary Calcium H and K lines in the spectrum of the spectroscopic binary δ Ori led to the discovery of the interstellar medium by J. Hartmann in 1904 with the Potsdam refractor. Some steps in the discovery of young binary stars are recounted, starting with the paper of Joy and van Biesbroeck in 1944. The history of ideas regarding the origin of binary systems is also briefly reviewed, beginning with J. Michell's statistical argument in 1767 that many close visual pairs of stars must indeed form physical systems, and W. Herschel's definition of a binary star as “a real double star - the union of two stars that are formed together in one system, by the laws of attraction”.

scholarly journals Long Baseline Interferometry and Binary Stars

1983 ◽  
Vol 62 ◽  
pp. 191-201
Author(s):  
John Davis
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Current Status ◽  
Fundamental Properties ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Spectroscopic Binary ◽  
Future Plans ◽  
Intensity Interferometer

AbstractThe observations of α Vir with the Narrabri Stellar Intensity Interferometer demonstrated the potential of long baseline interferometry for the determination of fundamental properties of double-lined spectroscopic binary systems. Since the completion of the programme with the Narrabri instrument the Chatterton Astronomy Department has been conducting a study aimed at developing a stellar interferometer with limiting magnitude V ≳ +8 and maximum baseline ≳ 1 km (resolution at 500 nm ≲ 7 × 10−5 seconds of arc). The way in which a long baseline interferometer may be used in the study of binary stars is outlined, the requirements for this work are discussed, and the current status and future plans of the Chatterton Astronomy Department’s programme to develop a new long baseline interferometer are summarised.

scholarly journals On the Distribution of Young Spectroscopic Binary Stars Over the Major Semiaxes of their Orbits

1982 ◽  
Vol 69 ◽  
pp. 129-131
Author(s):  
E.I. Popova ◽  
A.V. Tutukov ◽  
B.M. Shustov ◽  
L.R. Yungelson
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Spectroscopic Binaries ◽  
Close Binary ◽  
Physical Parameters ◽  
Origin And Evolution ◽  
Spectroscopic Binary ◽  
Visible Spectra ◽  
Major Semiaxes ◽  
The Masses

About 60% of stars of the disc population in our Galaxy are close binary systems (CBS). Half of the known CBS are spectroscopic binary stars (Kraitcheva et al., 1978).To know the distribution of a correlation between the masses of CBS components and semiaxes of their orbits is necessary for the investigation of the origin and evolution of CBS. For such statistical investigations, a catalogue of CBS was compiled at the Astronomical Council. The catalogue is based on the 6th Batten catalogue (Batten, 1967), its extensions (Pedoussant and Ginestet, 1971; Pedoussant and Carquillat, 1973) and data published up to the end of 1980 (Popova et al., 1981). Now it is recorded on magnetic tape and contains data on 1041 spectroscopic binaries; 333 of them are stars with two visible spectra. The latter are mostly systems prior to mass exchange and the distribution of physical parameters in these systems reflects the distribution and presumably conditions at the time of formation. Using some assumptions, we can obtain for spectroscopic binaries masses of the components M1 and M2 (or the ratio q = M1/M2) and semiaxes of their orbits. Masses of components with the known sin i were obtained by the usual technique; when sin i was not known, masses were estimated from the spectra. We shall discuss here the distribution of CBS in the M-a plane.

scholarly journals Discovery and characterisation of long-period eclipsing binary stars from Kepler K2 campaigns 1, 2, and 3

2018 ◽  
Vol 616 ◽  
pp. A38 ◽  
Author(s):  
P. F. L. Maxted ◽  
R. J. Hutcheon
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Binary Star ◽  
Eclipsing Binaries ◽  
Star Model ◽  
Eclipsing Binary ◽  
Giant Stars ◽  
Long Period ◽  
Eclipsing Binary Stars

Context. The Kepler K2 mission now makes it possible to find and study a wider variety of eclipsing binary stars than has been possible to-date, particularly long-period systems with narrow eclipses. Aims. Our aim is to characterise eclipsing binary stars observed by the Kepler K2 mission with orbital periods longer than P ≈ 5.5 days. Methods. The ellc binary star model has been used to determine the geometry of eclipsing binary systems in Kepler K2 campaigns 1, 2 and 3. The nature of the stars in each binary is estimated by comparison to stellar evolution tracks in the effective temperature – mean stellar density plane. Results. 43 eclipsing binary systems have been identified and 40 of these are characterised in some detail. The majority of these systems are found to be late-type dwarf and sub-giant stars with masses in the range 0.6–1.4 solar masses. We identify two eclipsing binaries containing red giant stars, including one bright system with total eclipses that is ideal for detailed follow-up observations. The bright B3V-type star HD 142883 is found to be an eclipsing binary in a triple star system. We observe a series of frequencies at large multiples of the orbital frequency in BW Aqr that we tentatively identify as tidally induced pulsations in this well-studied eccentric binary system. We find that the faint eclipsing binary EPIC 201160323 shows rapid apsidal motion. Rotational modulation signals are observed in 13 eclipsing systems, the majority of which are found to rotate non-synchronously with their orbits. Conclusions. The K2 mission is a rich source of data that can be used to find long period eclipsing binary stars. These data combined with follow-up observations can be used to precisely measure the masses and radii of stars for which such fundamental data are currently lacking, e.g., sub-giant stars and slowly-rotating low-mass stars.

scholarly journals Origin of the orbital period change in contact binary stars

2019 ◽  
Vol 28 (06) ◽  
pp. 1950044 ◽  
Author(s):  
V. V. Sargsyan ◽  
H. Lenske ◽  
G. G. Adamian ◽  
N. V. Antonenko
Keyword(s):  
Orbital Period ◽  
Binary Stars ◽  
Binary Systems ◽  
Binary Star ◽  
Period Change ◽  
Mass Asymmetry ◽  
Contact Binary Stars ◽  
Contact Binary ◽  
Energy Formula ◽  
Orbital Periods

The evolution of contact binary star systems in mass asymmetry (transfer) coordinate is considered. The orbital period changes are explained by an evolution in mass asymmetry towards the symmetry (symmetrization of binary system). It is predicted that decreasing and increasing orbital periods are related, respectively, with the nonoverlapping and overlapping stage of the binary star during its symmetrization. A huge amount of energy [Formula: see text][Formula: see text]J is converted from the potential energy into internal energy of the stars during the symmetrization. As shown, the merger of stars in the binary systems, including KIC 9832227, is energetically an unfavorable process. The sensitivity of the calculated results to the values of total mass and orbital angular momentum is analyzed.

scholarly journals Circumbinary Planets and the SOLARIS Project

2011 ◽  
Vol 7 (S282) ◽  
pp. 111-116 ◽  
Author(s):  
Maciej Konacki ◽  
Piotr Sybilski ◽  
Stanisław K. Kozłowski ◽  
Milena Ratajczak ◽  
Krzysztof G. Hełminiak
Keyword(s):  
South America ◽  
Binary Stars ◽  
Extrasolar Planets ◽  
Binary Star ◽  
Multiple Star ◽  
Eclipsing Binary ◽  
Stellar Astronomy ◽  
Eclipsing Binary Stars ◽  
Spectroscopic Binary ◽  
Circumbinary Planets

AbstractExtrasolar planets in binary and multiple star systems have become a noticeable niche with about 50 planets among over 500 known. Here we however focus on a particular subset of exoplanets in binary star systems — circumbinary planets. They have the unique advantage that a search for circumbinary planets does also significantly contribute to the understanding of their parent stars. We review what is currently known about circumbinary planets and then introduce our two projects aimed at detecting circumbinary planets: The TATOOINE project to find circumbinary planets around non-eclipsing double-lined spectroscopic binary stars with precision radial velocities, and the SOLARIS project to detect circumbinary planets with the timing of eclipses of eclipsing binary stars. For the SOLARIS project, we were granted 2.6 million USD to establish a network of at least four robotic 0.5-m telescopes on three continents (Australia, Africa and South America) to carry out precision photometry of a sample of eclipsing binary stars. We expect that both projects will have a large impact also on the observational stellar astronomy.

scholarly journals Адам и Ева, единосъщите – модел и мит на първата библейска двойка в българския междувоенен роман

2016 ◽  
Vol 16 ◽  
pp. 422-437
Author(s):  
Аглика [Aglika] Попова [Popova]
Keyword(s):  
Comparative Analysis ◽  
History Of Ideas ◽  
Prominent Feature ◽  
Garden Of Eden ◽  
Adam And Eve ◽  
The Bible ◽  
History Of ◽  
Christian Family ◽  
Definition Of ◽  
Point Of Intersection

Adam and Eve, consubstantial: Model and myth of the first Biblical couple in Bulgarian interwar novelThe article examines the first biblical couple as a tool for comparative analysis of the mod­ernist tendencies of Bulgarian novel in the period between the two World Wars. The research focuses on works by Chavdar Mutafov, Anna Kamenova, and Dimitar Dimov, along with examples taken from French and Romanian literary pieces as representatives of the wider, European history of ideas. In the image of Creation, but also the image of the original sin, Adam and Eve are of interest because of their unity, which eventually becomes the basis of the Christian family after they leave the Garden of Eden. The borders of the model given in the Bible are breached with the introduction of a new reading – the figures of Creation can now also be seen as figures of salvation. The knowledge gained by the existing studies of myth in European literature thus becomes the foundation for a revision of the hitherto selective interpretation of works by the Bulgarian novelists. The point of intersection between the dif­ferent approaches towards the first couple is their arduous integration into the surrounding world, and adaptation to the passage of time. Another prominent feature is the discussion about the possible development of the model; the newly introduced definition of salvation that comes after Creation and the fall of man. Adam i Ewa współistotni – model i mit pierwszej biblijnej pary w bułgarskiej powieści międzywojennejTematem artykułu jest pierwsza biblijna para ludzi, rozumiana jako wiodący motyw analizy porównawczej modernistycznych tendencji w bułgarskiej powieści okresu międzywojennego. Jako przykład posłużyły prace Czawdara Mutafowa, Anny Kamenowej i Dimityra Dimowa, a także francuskie i rumuńskie utwory literackie, służące osadzeniu wywodu w szerszym kontekście europejskiej historii idei. Zarówno w obrazie Stworzenia, jak i w obrazie grze­chu pierworodnego, postacie Adama i Ewy są interesujące ze względu na ich jedność, która ostatecznie staje się podstawą chrześcijańskiej rodziny po opuszczeniu przez nich rajskiego ogrodu. Granice modelu podanego w Biblii zostają naruszone przez wprowadzenie nowego odczytania – figury Stworzenia mogą być również odczytywane jako figury zbawienia. Wiedza zdobyta dzięki dotychczasowym studiom nad mitem w literaturze europejskiej staje się pod­stawą do rewizji selektywnej interpretacji bułgarskich powieściopisarzy. Punktem wspólnym dla różnych podejść w badaniu pierwszej pary ludzi jest ich trudna integracja z otaczającym światem i próba pogodzenia się z upływem czasu. Inną istotną cechą jest dyskusja na temat rozwoju tego modelu: nowo wprowadzona definicja zbawienia, które przychodzi po Stworzeniu i upadku człowieka.

scholarly journals Asteroseismology of Close Binary Stars: Tides and Mass Transfer

2021 ◽  
Vol 8 ◽  
Author(s):  
Zhao Guo
Keyword(s):  
Mass Transfer ◽  
Binary Stars ◽  
Binary Systems ◽  
Binary Star ◽  
Close Binary ◽  
Close Binaries ◽  
Linear Mode ◽  
Stellar Oscillations ◽  
Theoretical Approaches ◽  
Stellar Interiors

The study of stellar oscillations allows us to infer the properties of stellar interiors. Meanwhile, fundamental parameters such as mass and radius can be obtained by studying stars in binary systems. The synergy between binarity and asteroseismology can constrain the parameter space of stellar properties and facilitate the asteroseismic inference. On the other hand, binarity also introduces additional complexities such tides and mass transfer. From an observational perspective, we briefly review the recent advances in the study of tidal effects on stellar oscillations, focusing on upper main sequence stars (F-, A-, or OB- type). The effect can be roughly divided into two categories. The first one concerns the tidally excited oscillations (TEOs) in eccentric binaries where TEOs are mostly due to resonances between dynamical tides and gravity modes of the star. TEOs appear as orbital-harmonic oscillations on top of the eccentric ellipsoidal light curve variations (the “heartbeat” feature). The second category is regarding the self-excited oscillations perturbed by static tides in circularized and synchronized close binaries. It includes the tidal deformation of the propagation cavity and its effect on eigenfrequencies, eigenfunctions, and the pulsation alignment. We list binary systems that show these two types of tidal effect and summarize the orbital and pulsation observables. We also discuss the theoretical approaches used to model these tidal oscillations and relevant complications such as non-linear mode coupling and resonance locking. Further information can be extracted from the observations of these oscillations which will improve our understanding of tides. We also discuss the effect of mass transfer, the extreme result of tides, on stellar oscillations. We bring to the readers' attention: (1) oscillating stars undergoing mass accretion (A-, F-, and OB type pulsators and white dwarfs), for which the pulsation properties may be changed significantly by accretion; (2) post-mass transfer pulsators, which have undergone a stable or unstable Roche-Lobe overflow. These pulsators have great potential in probing detailed physical processes in stellar interiors and mass transfer, as well as in studying the binary star populations.

scholarly journals Effect of binary evolution on the inferred initial and final core masses of hydrogen-rich, Type II supernova progenitors

2020 ◽  
Vol 645 ◽  
pp. A6
Author(s):  
E. Zapartas ◽  
S. E. de Mink ◽  
S. Justham ◽  
N. Smith ◽  
M. Renzo ◽  
...  
Keyword(s):  
Mass Distribution ◽  
Binary Systems ◽  
Binary Star ◽  
Age Dating ◽  
Close Binary ◽  
Type Ii ◽  
Core Mass ◽  
History Of ◽  
Binary Evolution ◽  
The Impact

The majority of massive stars, which are the progenitors of core-collapse supernovae (SNe), are found in close binary systems. In a previous work, we modeled the fraction of hydrogen-rich, Type II SN progenitors whose evolution is affected by mass exchange with their companion, finding this to be between ≈1/3 and 1/2 for most assumptions. Here we study in more depth the impact of this binary history of Type II SN progenitors on their final pre-SN core mass distribution, using population synthesis simulations. We find that binary star progenitors of Type II SNe typically end their life with a larger core mass than they would have had if they had lived in isolation because they gained mass or merged with a companion before their explosion. The combination of the diverse binary evolutionary paths typically leads to a marginally shallower final core mass distribution. In discussing our results in the context of the red supergiant problem, that is, the reported lack of detected high luminosity progenitors, we conclude that binary evolution does not seem to significantly affect the issue. This conclusion is quite robust against our variations in the assumptions of binary physics. We also predict that inferring the initial masses of Type II SN progenitors by “age-dating” their surrounding environment systematically yields lower masses compared to methods that probe the pre-SN core mass or luminosity. A robust discrepancy between the inferred initial masses of a SN progenitor from those different techniques could indicate an evolutionary history of binary mass accretion or merging.

scholarly journals On the Development of Palinurus vulgaris, the Rock Lobster or Sea Crayfish

1891 ◽  
Vol 2 (2) ◽  
pp. 141-150 ◽  
Author(s):  
J. T. Cunningham
Keyword(s):  
Anterior Extremity ◽  
Historical Review ◽  
The State ◽  
The Body ◽  
Rock Lobster ◽  
Lower Lip ◽  
The World ◽  
History Of ◽  
Definition Of ◽  
Comparative Embryology

1. Historical Review.The history of our knowledge of this subject is complicated and curious, and is not quite correctly narrated in any English publication, not even by Balfour in his account of the development of Crustacea (Comparative Embryology, vol. i). The story begins with the establishment and definition of the genus Phyllosoma by Leach in 1818. Various succeeding zoologists included descriptions of species of Phyllosoma in their works, but the result of all previous investigations are included by Milne Edwards in the comprehensive account of the genus given in his Hist. Nat. des Crustacés, vol. ii, 1837. The state of knowledge at that time may be briefly summarised as follows:—The Crustaceans known by the name Phyllosoma had been found near the surface of the ocean in various parts of the world. They varied in size from less than half an inch to two inches. They were, when alive, of glassy transparency; the body was remarkably flat, and expanded horizontally, while the limbs were long, slender, and biramous. The body consisted of three parts; firstly, a head having the form of an oval leaf, bearing at its anterior extremity a pair of eyes on long stalks and two pairs of simple antennæ. The mouth was situated beneath the middle or posterior third of the head, and surrounded by an upper and lower lip, a pair of maxillæ, and the first pair of maxillæ. The second pair of maxillæ and the first pair of maxillipeds were rudimentary and situated behind the mouth. The second part of the body was the thorax, quite as flat but not so large as the head; it was usually broader than long.

scholarly journals DIVISION G COMMISSION 42: CLOSE BINARY STARS

2015 ◽  
Vol 11 (T29A) ◽  
pp. 474-489
Author(s):  
Mercedes T. Richards ◽  
Theodor Pribulla ◽  
Ignasi Ribas ◽  
David H. Bradstreet ◽  
Horst Dreschsel ◽  
...  
Keyword(s):  
Binary Stars ◽  
Close Binary ◽  
General Assembly ◽  
Vice Presidents ◽  
Double Stars ◽  
Close Binary Stars ◽  
Assistant Director ◽  
History Of ◽  
General Secretary

Commission 42 began life as Photometric Double Stars in 1948 at the 7th General Assembly in Zurich, under the presidency of Zdenek Kopal. As early as 1961, then General Secretary Lukas Plaut recommended a merger between C42 and C26, Double Stars, one of the original 32 commissions going back to 1919-22 (first president Aitken, assistant director at Lick). C42 became Close Binary Stars in 1970, at the 14th GA in Brighton (the first one I attended). Table 1 shows the presidents of C42, and vice presidents, from when the office started, through the history of the Commission.

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