61. IAU Commission 42 INTERNATIONAL ASTRONOMICAL UNION COMMISSION 42. CLOSE binary stars (ETOILES BINARIES SERREES). Together with Commission 27 Variable http://www.konkoly.hu/IAUC42/

INTERNATIONAL ASTRONOMICAL UNION COMMISSION 42. CLOSE BINARY STARS (ETOILES BINARIES SERREES) Together with Commission 27: Variable Stars , Commission 42 is part of Division V: Variable Stars of the International Astronomical Union The Web page of Commission 42 is valid for the term 2003 to 2006 and maintained by Andras Holl and Attila Sragli at Konkoly Observatory , Hungary. Last change made on Tuesday April 20 13:38:48 MEST 2004.

62. Binary Stars 1998 Aug 07 binary stars. In 1650 the Italian Jesuit Giovanni Riccioli observed that Mizar, one of two stars in the handle of Ursa Major long used as a test of visual acuity http://www.physics.uq.edu.au/people/ross/phys2080/binary/binaries.htm

BINARY STARS In 1650 the Italian Jesuit Giovanni Riccioli observed that Mizar, one of two stars in the handle of Ursa Major long used as a test of visual acuity, itself had a very close companion. The odds of two stars of similar brightness appearing so close together is too small not to suspect that the stars are actually physically close together, not like the chance grouping of Mizar and the fainter more distant of the pair Alcor. In the following years many such double stars were discovered and by 1804 William Herschel discovered that the fainter component of Castor (Castor B) had moved relative to the brighter component (Castor A), the first proof that gravity worked outside the solar system and the stars were gravitationally bound, visual binary stars In 1889 Pickering found that the spectral lines of the brighter component of Mizar (Mizar A) were usually double and the spacing varied with a regular 104 day period, the first spectroscopic binary to be discovered. Immediately after the discovery of the spectroscopic binary Mizar, Algol the demon star , beta Persei, was discovered to be a spectroscopic binary introducing the most important class of binary stars the eclipsing binary.

63. MSN Encarta - Binary Star I. Introduction. Binary Star, two stars that are bound to each other by gravity and orbit about a common center of mass. Importance of binary stars to Astronomy. http://encarta.msn.com/encyclopedia_761586362/Binary_Star.html

MSN Home My MSN Hotmail Shopping ... Money Web Search: logoImg('http://sc.msn.com'); Encarta Subscriber Sign In Help Home ... Upgrade to Encarta Premium Search Encarta Subscription Article MSN Encarta Premium: Get this article, plus 60,000 other articles, an interactive atlas, dictionaries, thesaurus, articles from 100 leading magazines, homework tools, daily math help and more for $4.95/month or $29.95/year (plus applicable taxes.) Learn more. This article is exclusively available for MSN Encarta Premium Subscribers. Already a subscriber? Sign in above. Binary Star I. Introduction Binary Star , two stars that are bound to each other by gravity and orbit about a common center of mass. Binary star systems are quite common and the... II. Classification of Binary Star Systems III. Interacting Binary Systems IV. Importance of Binary Stars to Astronomy Related Items Star black and white dwarf stars 50 items Multimedia Want more Encarta? Become a subscriber today and gain access to: Daily Math Help Literature Guides Researcher Tools Paper-Writing Guides 60,000 + articles

64. Binary Stars And Accretion Disks AS 4024 binary stars and Accretion Disks. Keith Horne, University of St.Andrews. Introduction to Close binary stars. (Hilditch). CUP . fetchbook . Amazon . http://star-www.st-and.ac.uk/~kdh1/bsad/bsad.html

AS 4024 Binary Stars and Accretion Disks Keith Horne, University of St.Andrews Astronomy Picture of the Day Introduction to Close Binary Stars. (Hilditch). CUP fetchbook Amazon Binary Star Lectures: 1.pdf .ps 1c.pdf .ps . Overview, circular orbit, types of binaries. 2.pdf .ps 2.pdf .ps . Gravity, energy and angular momentum conservation, Kepler's law, conics. 3.pdf .ps 3c.pdf .ps . 2-body problem, centre of mass, reduced mass, relative and barycentric orbits. 4.pdf .ps 4c.pdf .ps . radial potential, turning points, orbit shape, speed, true,eccentric,mean anomalies, Kepler's equation. 5.pdf .ps 5c.pdf .ps . orbit orientation, radial velocity orbits, minimum masses, cross-correlation velocities, periodograms. 6.pdf .ps 6c.pdf .ps . pulse timing orbits, inclinations from astrometry, eclipses, polarimetry. 7.pdf .ps 7c.pdf .ps . perturbed 2-body motion, Lagrange equations, apsidal motion. 8.pdf .ps 8c.pdf .ps . non-spherical potentials, equilibrium and dynamical tides, Zahn synchronisation and circularisation timescales. 9.pdf

65. Binary Stars binary stars. They stepped out into the night, together, always. They were sisters, a year apart, telepathic and their skin was moonlight white. http://takingcareofbusiness.com/rawether/binary_stars.htm

Binary Stars They stepped out into the night, together, always. They were sisters, a year apart, telepathic and their skin was moonlight white. They went out into the night together. Not every night, not the nights their dad fell asleep on the couch watching porn, the zipper to his pants gaping, showing curly hair, when he'd wake up and sit up. We turn off the television because we think it might wake him up and get him to go to bed so we can go out. He wakes up when we turn off the television. Sometimes when dad wakes up and stands and stretches his arms way up we see his round belly, pink and hairy when his sweatshirt rides his arms up. He speaks some other language, he does. At night, only at night though, dad has a language for day and for night, as do we sisters. We go out at night because at night we don't have to be two separate people. We can be what we were meant to be- Siamese twins. We go out at night and tie our ankles together, our wrists. Sometimes, when there's enough time before dark, we write down our lines so that we can practice having us each speak every other word. We want to be like real twins, but better. We want to have these two heads, not grown together like most twins. And we don't want to share one brain, we want to have our two but they'll still be connected to each other in some way by our stars. We're gonna feel our connection like we sometimes feel invisible tails, helping us through the trees when we climb together. One of us likes climbing more than the other. We have a weak right arm. It shattered when we were young, one younger. We were new at it then. When Dad wasn't watching porn, he showed us

66. A Ritzian Interpretation Of Variable Stars In 1913 Willem de Sitter urged abandonment of the Ritz theory because binary stars (the interstellar medium scenario) failed to show the predicted c + v http://www.ebicom.net/~rsf1/binaries.htm

Home Up one level Previous Next This article has the following sections. A Ritzian Interpretation of Variable Stars - You are here! Non-pulsating Cepheid Variables Ritzian Gamma-Ray Bursts Ultra High Energy Cosmic Rays Modeling Geminga ... GRB 790731 and omega Geminorum A Ritzian Interpretation of Variable Stars An enlargement on 1987-1989 researches by V.I. Sekerin and M.S. Serbulenko Installed 05 Jan 1999 - Latest Update 15 May 2004 (Newly added or modified material is in bold.) Keywords: Close Binary Stellar Systems, Variable Star, Gamma-Ray Bursts, Speed of Light This article is written under the presumption that the constancy of the "measured" speed of light by all observers (in vacuo) is an unresolved issue. The author favors Ritz's use of c+v relativity but with the reservation that extinction (Tolman or Ewald-Oseen), i.e., the speed of light eventually reaches a terminal speed with respect to any given medium, has to be taken into account. De Sitter's (1913) argument against Ritz is used as a theoretical springboard from which to examine currently published observations of what are thought to be radially pulsating variable stars. High-angular-resolution photographs of these variables obtained from the Hubble Space Telescope (HST), the very large array (VLA) radio telescope(s), the growing family of very large telescopes (VLTs), and/or the publication of light curves along with phase-matched spectroscopic line profiles (absorption and emission) can be used to resolve the

67. Binary Star Modeling: Event Proceedings New Generation Modeling Developments and Results for binary stars. Combined Spectrum Synthesis and Light Synthesis Analysis of Eclipsing binary stars. http://www.ucalgary.ca/~milone/AAS97/event_proceedings.html

New Generation Modeling Developments and Results for Binary Stars Event Proceedings Opening Remarks: Enlightening Light Curves or Modeling for the Masses Remarks by: E.F. Milone, Co-Director of the RAO. University of Calgary. Calgary, Alberta, Canada. The advances in the modeling of eclipsing binary light curves (generically including polarimetric, spectrophotometric, and radial velocity curves, spectral line profiles, spectral indices, and other observables) were last reviewed comprehensively in 1991 at IAU sessions in Argentina. The field has continued to develop, and since light curve models and codes are depended on to produce reliable radii and masses, among other fundamental stellar properties, it is appropriate to review what is new in both models and the programs to implement them. The new model improvements include more realistic spot simulations, radiative transfer treatment of eclipses by translucent atmospheric clouds, improved radiation interactions between the components, non-linear limb-darkening, and non-solar metallicities. Codes are now available with improved integration and convergence techniques, and are modularized to permit added operations. The session is designed to illustrate these advances and the benefits for binary star research. Slide 1: Al Phoenicis: Spectra of the Residuals, from above.

68. Binary Stars -- From Eric Weisstein's World Of Astronomy About this site. Stars , binary stars v. binary stars, binary stars are stars which are gravitationally bound to each other and which orbit the center of mass. http://scienceworld.wolfram.com/astronomy/BinaryStars.html

Stars Binary Stars Binary Stars Binary stars are stars which are gravitationally bound to each other and which orbit the center of mass. Binary stars may be detected by brightness variations when their orbital plane is along the line of sight so that one eclipses the other ( eclipsing binary ), spectral changes as one star occults the other ( spectroscopic binary ), high angular resolution interferometric measurements, or visually if sufficiently separated ( visual binary Cataclysmic Variable Eclipsing Binary Spectroscopic Binary ... Visual Binary

69. Binary Stars Contents binary stars. The SPH particles, like before. The code can also handle binaries for which the stars have different masses. http://www.astro.northwestern.edu/StarCrash/manual/html/node20.html

Next: Finishing Relaxation Up: Relaxation Previous: Single Stars Contents Binary Stars The SPH code has routines to create binaries with both irrotational and corotating velocity profiles. For the former case, there is no fixed reference frame in which the material is stationary, and we have not yet implemented a way to relax the matter configuration exactly. For ways of calculating these configurations, see, e.g., Gourgoulhon et al. (2001) Taniguchi et al. (2001) , and references therein. On the other hand, binary stars in corotation, also known as synchronized binaries, can be relaxed, since they are static in a frame which rotates with the same angular frequency as the matter. For this case, called by setting the parameter NRELAX =2, the code adds in a false centrifugal force, to handle the rotation of the frame, yielding a force law for quantities in the corotating frame where we calculate the corotating frame's angular velocity by taking the average of the net forces on each component of the binary divided by the distance from the origin to the center of mass of each component. Note that this routine works for a given binary separation, which is given by the input parameter . After each timestep, we shift the positions of both stars very slightly to keep the center of mass separation at the proper value, with the system center of mass at the origin. It is possible to edit the code to produce a relaxed sequence with a smoothly varying separation, by defining a new separation variable and replacing references to

70. World Builders Binary Stars And The Center Of Mass binary stars travel with a partner, another star that is linked to them by gravity. The stars do not orbit around each other. Here is a pair of binary stars http://curriculum.calstatela.edu/courses/builders/lessons/less/les1/binary_stars

Your browser does not support script World Builders™ World Builders™ Session One Astronomy Session One Astronomy Binary Star Systems Binary Star Systems The stars orbit around their common center of mass. Some of the stars in the universe are members of binary star systems. My sources give different percentages, but there are enough of them so that you could plan for a binary star system for your worlds. Binary stars travel with a partner, another star that is linked to them by gravity. The stars do not orbit around each other. They orbit around their common center of mass The center of mass is where the fulcrum would be if the stars were balanced on a seesaw. This is how it works with people. The weight is the same and the distance is the same on each side. The board is horizontal because . . the weights and the distances are the same on both sides of the Center of Balance. Now let's do it with stars. Here is a pair of binary stars: Each star has about the same mass as our sun.

71. World Builders Introduction To Binary Stars And Twin Planets World Builders™ World Builders™. Session One Astronomy Session One Astronomy. binary stars and Twin Planets binary stars and Twin Planets. http://curriculum.calstatela.edu/courses/builders/lessons/less/les1/binary_intro

Your browser does not support script World Builders™ World Builders™ Session One Astronomy Session One Astronomy Binary Stars and Twin Planets Binary Stars and Twin Planets Gravitational forces govern the relationships between stars and planets. The relationships between objects in space are governed by gravitational forces. Matter has mass, and mass is associated with gravity. Large bodies, such as stars, have a lot of gravitational attraction, and it is the sun's gravity that keeps the planets from just wandering away into space. The gravity of the earth and the gravity of the moon affect each other's orbits, hold the two bodies together, and generate tides. Gravity is a very important force, and astronomers and physicists have developed formulas that describe what it does. However, so far, we do not know what gravity really is or why it works. Scientists of the future, here is a challenge for you! When stars form, sometimes they form as one star in the center of a protoplanetary disk, but sometimes two or more stars may form there. Many of the stars that we see appear to be members in stellar groupings. Two stars that are bound to each other gravitaionally are called binary stars, and larger groups of three, four, or even five gravitationally linked stars have been reported. For us as world builders, our questions are about the interactions of stars and planets in these groups. Here is some information about how they work.

72. Astronomy Class Oct 01 Astronomy Class Oct 01. binary stars. More importantly, though, the behavior of binary stars teach us lots about the stars themselves. http://www.rpi.edu/dept/phys/Courses/Astro_F97/Class11/oct01.html

Astronomy Class Oct 01 Binary Stars This topic may sound like we're going off on a tangent, but in fact we're not. In the first place, about half the stars in the sky are part of binary or multiple systems. More importantly, though, the behavior of binary stars teach us lots about the stars themselves. We'll get our first glimpse at the physics that makes stars shine. Introduction Binary stars come in different combinations: Capella . Similar stars, close to each other. Sirius . One big bright star, and one "white dwarf". Kinds of binaries Spectroscopic binary motion Example: HD 48099 Orbital motion Zeilik Fig.12-3: Luminosity and mass Mass-Luminosity relationship New stuff: Lifetime of a star Eclipsing binary motion Example: RU Ursa Minoris Zeilik Fig.12-11: Radius and mass Stuff about stars: A Recap Studio exercise Today you will use the CUPS Astrophysics module on Binary Stars to simulate a spectroscopic binary and an eclipsing binary. You will use the program to determine the orbit parameters of two actual binary stars. First, connect to the CUPS modules in the

73. Binary Stars Links Science Astronomy Stars binary stars. fun! binary stars Web Search Results Below (Add Your Site or modify). Astronomical http://www.zookle.com/Science/Astronomy/Stars/Binary_Stars/

zOO KLE link exchange top 100 Add Your Site Jokes ... binary music star Links: Science: Astronomy: Stars: Binary Stars Home Science Astronomy Stars : Binary Stars Buy Binary Star Music At Amazon.com and Save! Would you like to save on Binary Star Music and CDs at Amazon and other stores? Compare prices at BookSellersNow.com! Our site continually proves that online shopping can be fun! Binary Stars Web Search Results Below Add Your Site or modify Astronomical League Double Star Club The purpose of the Double Star Club is to introduce observers to 100 of the finest double and multiple stars in the heavens. http://www.astroleague.org/al/obsclubs/dblstar/dblstar1.html Astronomy 101/103 Web Simulations Includes two JAVA simulations of binary star systems. http://instruct1.cit.cornell.edu/courses/astro101/java/simulations.htm Binary Star Simulation This is a representation of the binary star on a graphical and easy way. http://instruct1.cit.cornell.edu/courses/astro101/java/binary/binary.htm Binary Stars Astronomy Lecture A single introductory astronomy lecture on Binary Stars, including several useful diagrams. http://zebu.uoregon.edu/~js/ast122/lectures/lec11.html

74. Simulations Of Mass Transfer In Binary Stars Simulations of Mass Transfer in binary stars. Introduction As a star exhausts its supply of hydrogen for fueling its internal nuclear http://www.princeton.edu/~ratliff/research/research.html

Simulations of Mass Transfer in Binary Stars Introduction: As a star exhausts its supply of hydrogen for fueling its internal nuclear reactions, it begins to swell in size as the surface layers become cool and reddened. Eventually, the star can become a red giant, many times larger than its size while in the hydrogen-burning phase of its life. If such a star happens to be a member of close binary system where two stars orbit about one another, it may be possible that the star becomes so distended that the surface layers feel a stronger gravitational attraction from the companion star than from the star to which they belong. In this case, the companion star is able to pull a stream of gas away from the giant star and onto itself. If the two stars are close enough, the stream actually impacts the companion star driving the temperatures in the gas up to millions of degrees Kelvin. After impact the material is reflected and begins to orbit the star forming an accretion disk. Description: Below is an image of the results of a two dimensional hydrodynamical simulation of just such a system

75. Starfire Optical Range - Imagery (Binary Stars - More Binary Stars) home / imagery / more binary stars binary stars in. Ursa Major, Cancer, and Delphinus. As explained in detail in The Astronomical http://www.de.afrl.af.mil/SOR/binary2.htm

Imagery Asteroids (Vesta and Ceres) Binary Stars Beta Del k-Peg more binary stars Capella Hyakutake Comet Leonids Meteor Trails Saturn ... imagery / more binary stars Binary Stars in Ursa Major, Cancer, and Delphinus As explained in detail in The Astronomical Journal for January 2000, (Volume 119, pages 378-389), the Starfire Optical Range made extensive observations of selected binary stars, both with and without a guide star laser. The binaries are shown below, where a star observed without adaptive optics would occupy the entire field of view in each image. 10 Ursae Majoris had a separation of 0.498±0.004 arc seconds and a large magnitude difference of 1.783±0.021. phi Ursae Majoris was separated by 0.245"±0.002", with a magnitude difference of 0.277±0.026. 81 Cancri was barely resolved at 0.123"±0.001", and its magnitude difference of -0.120±0.042, indicates that the historically fainter companion is brighter at the wavelength of observation here, 0.85 microns. kappa Ursae Majoris, at a separation of 0.067"±0.001" and a magnitude difference of 0.63±0.14 magnitudes, only shows an elongation, but through detailed mathematical processing its parameters are determined. Based on this observation and other recent high-resolution measurements, a new orbit has been derived for this pair.

76. The Lives Of Binary Stars the lives of binary stars, next page. http://www.shef.ac.uk/physics/people/vdhillon/seminars/sas/title.html

the lives of binary stars a brief history of binary stars the birth of binary stars the binary star zoo the evolution of binary stars ... why study binaries? Vik Dhillon, University of Sheffield 22 October 2001

77. Tidal Evolution And Oscillations In Binary Stars Third Granada Workshop on Stellar Structure. Tidal Evolution and Oscillations in binary stars. Tidal Evolution and Oscillations in binary stars http://www.iaa.es/~claret/tidal/tidal2004.html

Third Granada Workshop on Stellar Structure Tidal Evolution and Oscillations in Binary Stars Workshop organized by the Instituto de Astrofisica de Andalucia Granada , Spain, May 26-28 , 2004 FINAL ANNOUNCEMENT The scientific programme and speakers are given in this announcement. The list of participants with their affiliations and e-mail addresses as well as the talk/poster list are also included. A interactive map of Granada has been put in this announcement in order to help you to find your way around (see also the section Conference venue and facilities ). The complete list of the social events is also given. GENERAL INFORMATION An international workshop on the theoretical and observational problems of tidal evolution and oscillations in binary stars is to be held in Granada, Spain, from May 26-28 , 2004. This workshop is being organized by the Instituto de Astrofisica de Andalucia (IAA, CSIC) with support from the Spanish Consejo Superior de Investigaciones Cientificas (CSIC) . In addition, Commissions 35 (Stellar Structure) and 42 (Close Binaries) have expressed their support to the scientific objectives of the workshop.

78. A Triplet Of Binary Stars A triplet of binary stars. In the binary star system GX 1+4, the compact object is a neutron star, which is even smaller and denser than a white dwarf. http://www.physics.usyd.edu.au/rcfta/anrep96/anrep96/node14.html

Next: Electrically powered solar flares Up: Research highlights Previous: Shocking dirt between the A triplet of binary stars Binary star systems where one of the stars is the remnant of an ordinary star which has finished ``burning'' its fuel, are the subject of three widely different projects by Michelle Storey, Kinwah Wu and Jenny Nicholls. The mechanism behind the variable non-thermal radio emission from the binary star system V471 Tauri, which comprises a white dwarf and a main sequence companion star, is being investigated by Michelle Storey and Jenny Nicholls. Recent observations indicate that the radio emission from V471 Tauri varies as the two stars orbit each other, with a drop in intensity as the white dwarf is eclipsed by its companion. The intensity variation suggests that there is a region of enhanced emission between the two stars which is periodically obscured by the main sequence star. Both stars are thought to have magnetic fields, with that of the main sequence star dominating the region between the two stars. Michelle and Jenny suggest that as the magnetic fields of the two stars interact they accelerate electrons to mildly relativistic energies, producing a greater density of mildly relativistic electrons in the region between the two stars than elsewhere in the system. It is this higher density of electrons that gives rise to the higher levels of radio emission. Michelle and Jenny have calculated the emission from a system with a simple dipole field, a region of enhanced electron density between the two stars and a magnetized wind, and find that the model can fit the data provided the region of enhanced density is a wide wedge.

79. Science Search > Binary Stars 2059. 4. binary stars Astronomy Lecture A single introductory astronomy lecture on binary stars, including several useful diagrams. http://www.science-search.org/index/Astronomy/Stars/Binary_Stars/

Search for: Current Category Everything What's new Top Searches Statistics Science News ... Home Current location: Astronomy Stars > Binary Stars Binary Star Simulation This is a representation of the binary star on a graphical and easy way. http://instruct1.cit.cornell.edu/courses/astro101/java/binary/binary.htm detailed information Rating: [7.00] Votes: [1743] Astronomical League Double Star Club The purpose of the Double Star Club is to introduce observers to 100 of the finest double and multiple stars in the heavens. http://www.astroleague.org/al/obsclubs/dblstar/dblstar1.html detailed information Rating: [6.00] Votes: [1468] Astronomy 101/103 Web Simulations Includes two JAVA simulations of binary star systems. http://instruct1.cit.cornell.edu/courses/astro101/java/simulations.htm detailed information Rating: [6.00] Votes: [2059] Binary Stars Astronomy Lecture A single introductory astronomy lecture on Binary Stars, including several useful diagrams. http://zebu.uoregon.edu/~js/ast122/lectures/lec11.html

80. Educational Observatory - Binary Stars binary stars What are the differeces between double stars, variable stars and binary stars? Eclipsing binary stars What are binary stars? http://www.edu-observatory.org/eo/binary_stars.html

Binary Stars What are the differeces between double stars variable stars and binary stars Eclipsing Binary Stars - What are Binary Stars? Most stars are found in groups of stars that are gravitationally bound with each other. The majority of these stars are found in binary systems which are systems of two stars in orbit around a common center of mass. One can classify binary stars based on their appearance from earth. Stars that are far enough apart to be distinguished from each other are known as visual binaries. Other binaries are too close and far away to be seen separately but can distinguished using the doppler shift of their spectra. These are spectroscopic binaries. Some of the "Astronomical Seeing" Scales Astronomical Seeing Fix: Chapter 21 Binary Star Systems Interactive Star Atlas ... The Formation of Binary Stars - Recent observational investigations of the frequency of occurrence of pre-main-sequence binary stars have reinforced earlier suspicions that "binary formation is the primary branch of the star-formation process". A number of different theories have been proposed to explain the preponderance of binary stars. Klein et al.

A  B  C  D  E  F  G  H  I  J  K  L  M  N  O  P  Q  R  S  T  U  V  W  X  Y  Z

Page 4     61-80 of 105    Back | 1  | 2  | 3  | 4  | 5  | 6  | Next 20