scholarly journals Isolated Binaries and Triples in N-body Systems

1995 ◽  
Vol 164 ◽  
pp. 372-372
Author(s):  
J. Anosova ◽  
L. Kiseleva
Keyword(s):  
Globular Cluster ◽  
Binary Stars ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Time Interval ◽  
Galactic Field ◽  
Multiple Stars ◽  
Binary And Multiple Stars ◽  
Marked Tendency ◽  
Triple Stars

Stars show a marked tendency to form the systems of different multiplicity starting from the smallest systems as binary and triple stars up to clusters with a significantly larger number of objects (N ~ 107 for globular cluster s). Different investigators have used different methods of binary stars identificati on but modern observations give a frequency of binary and multiple stars in the Galactic field up to 70% Binary and multiple stars are also often present within star clusters. It is therefore very important to be able to identify such systems as rather isolated substructures in which the dynamical evolution is not significantly affected by other stars (at least, during some considerab le time interval).

scholarly journals Long-Term Coudé Radial-Velocity Studies With a 1.2-m Telescope

2001 ◽  
Vol 183 ◽  
pp. 283-288
Author(s):  
C.D. Scarfe
Keyword(s):  
Radial Velocity ◽  
Binary Stars ◽  
Star System ◽  
Standard Star ◽  
Stellar Spectra ◽  
Multiple Stars ◽  
Binary And Multiple Stars ◽  
Selection Of

AbstractI have used the 1.2-m telescope and coudé spectrograph of the Dominion Astrophysical Observatory for more than 30 years in a program of radial-velocity observations of binary stars. The program was begun with photographic plates as detectors, but for 20 years the primary detector has been the radial-velocity scanner, which cross-correlates stellar spectra with an artificial mask.Since some of the binaries under observation have periods of several years, the instrument’s stability is an important consideration. I have therefore been obliged to observe standard stars and asteroids to check its performance. These observations are of relevance to efforts to improve the IAU standard star system.I will describe the telescope, spectrograph and scanner, and will briefly discuss some of the results obtained for a selection of binary and multiple stars.

scholarly journals A Catalogue of Nearby Wide Binary and Multiple Stars

1992 ◽  
Vol 135 ◽  
pp. 299-299
Author(s):  
A. Poveda ◽  
M.A. Herrera ◽  
C. Allen ◽  
G. Cordero ◽  
C. Lavalley
Keyword(s):  
Dynamical Evolution ◽  
Bright Star ◽  
Wide Binary ◽  
Multiple Systems ◽  
Star Catalogue ◽  
Multiple Stars ◽  
Nearby Stars ◽  
Binary And Multiple Stars

AbstractNo modern catalogue of wide binary and multiple systems (WBMS) exists for the region of the solar vicinity (stars nearer than ~22 pc), that include updated information on their membership to moving clusters and an age classification. With the aim of filling this gap, and also because of its importance for investigating the dynamical evolution of double and multiple systems, we have compiled a WBMS list extracted from the catalogues of nearby stars of Gliese (1969, also Gliese & Jahreiss 1979), as well as Luyten’s NLTT (Luyten 1979–1980, Luyten & Hughes 1980, see also Warren et al. 1989), the Bright Star Catalogue (Hoffleit 1982), the catalogue of Woolley et al. (1970) and other sources.By comparing the transverse velocities of WBM systems with those expected for members of the Hyades and Sirius Superclusters, membership of some WBMS to them has been established. We have classified as probably young systems (PYS) those with one component satisfying at least one of various criteria of youth. A system that is not a PYS is classified as probably old (POS).The catalogue contains 385 binaries and 85 systems of higher multiplicity. Out of these, 129 binaries are PYS and 256 are POS, while 32 multiples are PYS and 53 are POS.

scholarly journals COMMISSION 42: CLOSE BINARY STARS

2008 ◽  
Vol 4 (T27A) ◽  
pp. 260-266
Author(s):  
Slavek M. Rucinski ◽  
Ignasi Ribas ◽  
Alvaro Giménez ◽  
Petr Harmanec ◽  
Ronald W. Hilditch ◽  
...  
Keyword(s):  
Binary Stars ◽  
Close Binary ◽  
Close Binaries ◽  
Evolutionary Processes ◽  
Spring Meeting ◽  
Close Binary Stars ◽  
Multiple Stars ◽  
Short Period ◽  
Binary And Multiple Stars ◽  
Full Day

Two meetings of interest to close binaries took place during the reporting period: A full day session on short-period binary stars – mostly CV's – (Milone et al. 2008) during the 2006 AAS Spring meeting in Calgary and the very broadly designed IAU Symposium No. 240 on Binary Stars as Critical Tools and Tests in Contemporary Astrophysics in Prague, 2006, with many papers on close binaries [Hartkopf et al. 2007]. In addition, the book by Eggleton (2006), which is a comprehensive summary of evolutionary processes in binary and multiple stars, was published.

scholarly journals Habitable planet formation in extreme planetary systems: systems with multiple stars and/or multiple planets

2007 ◽  
Vol 3 (S249) ◽  
pp. 319-324
Author(s):  
Nader Haghighipour
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Planet Formation ◽  
Planetary Systems ◽  
Dynamical Evolution ◽  
Giant Planets ◽  
Habitable Planets ◽  
Multiple Stars ◽  
Habitable Zones ◽  
Habitable Planet

AbstractUnderstanding the formation and dynamical evolution of habitable planets in extrasolar planetary systems is a challenging task. In this respect, systems with multiple giant planets and/or multiple stars present special complications. The formation of habitable planets in these environments is strongly affected by the dynamics of their giant planets and/or their stellar companions. These objects have profound effects on the structure of the disk of planetesimals and protoplanetary objects in which terrestrial-class planets are formed. To what extent the current theories of planet formation can be applied to such “extreme” planetary systems depends on the dynamical characteristics of their planets and/or their binary stars. In this paper, I present the results of a study of the possibility of the existence of Earth-like objects in systems with multiple giant planets (namely υ Andromedae, 47 UMa, GJ 876, and 55 Cnc) and discuss the dynamics of the newly discovered Neptune-sized object in 55 Cnc system. I will also review habitable planet formation in binary systems and present the results of a systematic search of the parameter-space for which Earth-like objects can form and maintain long-term stable orbits in the habitable zones of binary stars.

scholarly journals Quantitative Spectroscopy of Close Binary Stars

2011 ◽  
Vol 7 (S282) ◽  
pp. 359-364 ◽  
Author(s):  
K. Pavlovski ◽  
J. Southworth
Keyword(s):  
Binary Stars ◽  
High Mass ◽  
Close Binary ◽  
Intermediate Mass ◽  
Intermediate Mass Stars ◽  
Close Binary Stars ◽  
Multiple Stars ◽  
Binary And Multiple Stars ◽  
Detached Binaries ◽  
Type Mass

AbstractThe method of spectral disentangling has now created the opportunity for studying the chemical composition in previously inaccessible components of binary and multiple stars. This in turn makes it possible to trace their chemical evolution, a vital aspect in understanding the evolution of stellar systems. We review different ways to reconstruct individual spectra from eclipsing and non-eclipsing systems, and then concentrate on some recent applications to detached binaries with high-mass and intermediate-mass stars, and Algol-type mass-transfer systems.

scholarly journals Binary Information from Open Clusters Using SEDS (BINOCS) Project: The Dynamical Evolution of the Binary Populations in Cluster Environments

2015 ◽  
Vol 12 (S316) ◽  
pp. 255-256
Author(s):  
Peter Frinchaboy ◽  
Benjamin Thompson
Keyword(s):  
Binary Stars ◽  
Binary Data ◽  
Binary Star ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Mass Range ◽  
Open Clusters ◽  
Stellar Clusters ◽  
Multi Wavelength ◽  
Binary Information

AbstractStudying the internal dynamics of stellar clusters is conducted primarily through N-Body simulations. One of the major inputs into N-Body simulations is the binary star frequency and mass distribution, which is currently constrained by relations derived from field binary stars. However to truly understand how clustered environments evolve, binary data from within star clusters is needed including masses. Detailed information on binaries masses, primary and secondary, in star clusters has been limited to date. The primary technique currently available has been radial velocity surveys that are limited in depth. Using previous two-band photometry-based studies that may cover different mass ranges produce potentially discrepant interpretations of the observed binary population. We introduce a new binary detection method, Binary INformation from Open Clusters Using SEDs (BINOCS) that covers the wide mass range needed to improve cluster N-body simulation inputs and comparisons. Using newly-observed multi-wavelength photometric catalogs (0.3 - 8 microns) of the key open clusters with a range of ages, we can show that the BINOCS method determines accurate binary component masses for unresolved cluster binaries through comparison to available RV-based studies. Using this method, we present results on the dynamical evolution of binaries from 0.4 - 2.5 solar masses within five prototypical clusters, spaning 30 Myr to 3.5 Gyr, and how the binary populations evolve as a function of mass.

scholarly journals Introduction & Overview to Symposium 240: Binary Stars as Critical Tools and Tests in Contemporary Astrophysics

2006 ◽  
Vol 2 (S240) ◽  
pp. 5-16 ◽  
Author(s):  
Edward F. Guinan ◽  
Petr Harmanec ◽  
William Hartkopf
Keyword(s):  
High Precision ◽  
Binary Stars ◽  
Binary Systems ◽  
New Technologies ◽  
Binary Star ◽  
Electromagnetic Spectrum ◽  
Multiple Star ◽  
Multiple Stars ◽  
Star Studies ◽  
Binary And Multiple Stars

AbstractAn overview is presented of the many new and exciting developments in binary and multiple star studies that were discussed at IAU Symposium 240. Impacts on binary and multiple star studies from new technologies, techniques, instruments, missions and theory are highlighted. It is crucial to study binary and multiple stars because the vast majority of stars (>60%) in our Galaxy and in other galaxies consist, not of single stars, but of double and multiple star systems. To understand galaxies we need to understand stars, but since most are members of binary and multiple star systems, we need to study and understand binary stars. The major advances in technology, instrumentation, computers, and theory have revolutionized what we know (and also don't know) about binary and multiple star systems. Data now available from interferometry (with milliarcsecond [mas] and sub-mas precisions), high-precision radial velocities (∼1-2 m/s) and high precision photometry (<1–2 milli-mag) as well as the wealth of new data that are pouring in from panoramic optical and infrared surveys (e.g., > 10,000 new binaries found since 1995), have led to a renaissance in binary star and multiple star studies. For example, advances have lead to the discovery of new classes of binary systems with planet and brown dwarf components (over 200 systems). Also, extremely valuable data about binary stars are available across the entire electromagnetic spectrum — from gamma-ray to IR space missions and from the ground using increasingly more powerful and plentiful optical and radio telescopes as well as robotic telescopes. In the immediate future, spectral coverage could even be extended beyond the radio to the first detection of gravity waves from interacting close binaries. Also, both the quality and quantity of data now available on binary and multiple stars are making it possible to gain unprecedented new insights into the structure, and formation and evolution of binary stars, as well as providing valuable astrophysical information (like precise stellar masses, radii, ages, luminosities and distances) to test and constrain current astrophysical theory. These major advances permit tests of current theories and ideas in stellar astrophysics and provide the foundations for the next steps in modeling and improvements in theory to be taken.

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