41. Binary Stars binary stars. One could think that stars are isolated celestial bodies, just likethe Sun. Actually, two thirds of the stars are gathered into multiple systems. http://www.pd.astro.it/hosted/MOSTRA/E-MOSTRA/NEW/A3042DOP.HTM

BINARY STARS One could think that stars are isolated celestial bodies, just like the Sun. Actually, two thirds of the stars are gathered into multiple systems. Most of them are binary systems (that is formed by two stars alone, like Sirius), but there exist systems formed by three, four and even six stars. These stars rotate around a common point, which is the baricenter of the system, each one describing an elliptical orbit. One focus of the ellipse coincides with the baricenter. In a binary system, the two stars move around the common baricenter, O. The ratio between their distances from the baricenter is inversely proportional to the ratio between their masses. One should not mistake physical binaries with optical doubles, that is those stars that are close to each other due to just a perspective effect (for example, Mizar and Alcor, the stars of the "tail" in Ursa Major). There are several different types of binary systems. Visual binaries are those systems where both components can be recognized with a telescope. The resolving power of telescopes is limited, so not all binary systems can be visually distinguished. However, the presence of two rotating stars can be revealed also in an indirect way. This is the case of

42. Binary Star Simulation ORBITING binary stars http://www.pas.rochester.edu/~dmw/ast102/Java/binary.htm

O RBITING B INARY S TARS Description Instructions Example to try Astronomy 101/103 Cornell University Terry Herter You need a JAVA enabled browser to view this simulation. This simulation is a bit unstable and may bring down the machine you are running. DESCRIPTION: Allows you to set the masses, orbital separation, orbital eccentricity, the inclination angle to our line of sight, and the angle of the nodes of an orbiting star pair. You see the privileged (from above the orbit) and the earth view of the system (which depends on the inclination angle). The observed velocities of the two stars, and the Doppler shifted spectral lines (as seen against the combined continuum from the two stars) are also shown in the upper right box. The spectral lines associated with each star are indicated and the unshifted line positions are also marked. The movement of the spectral lines against the continuum has been greatly exaggerated for display purposes, and the difference in brightness of the two stars has been ignored. We have the following definitions: Mass 1 or Mass 2 The mass of each of the two stars.

43. Research At The Bradstreet Observatory Research. At the Bradstreet Observatory, most of our research effortsare focused on photoelectric photometry of Eclipsing binary stars. http://www.eastern.edu/academic/trad_undg/sas/depts/physsci/research.html

Research At the Bradstreet Observatory, most of our research efforts are focused on photoelectric photometry of Eclipsing Binary Stars. Dr. David Bradstreet has written an article entitled "Ephemerides of Variable Stars" that explores this in depth. Ephemerides of Variable Stars (200K PDF) Ephemerides of Variable Stars (3MB Word document) Most recently, we have been studying the eclipsing classical nova V1494 Aql. This is a system which includes 2 stars, one of which is having gas dumped on it by the other. This system was still not at quiescence as of November 2001, and will continue to be studied as it becomes observable again. A poster was presented on our findings at the 2002 AAS meeting in Washington, DC. Click here for a copy of our V1494 Aql poster in PDF format. We are also continuing to study the close binary CM Dra in order to obtain precise timings of minimum light in search of third bodies (brown dwarfs of planets). We presented a poster of some of our work on this star system at the January 2001 AAS meeting in San Diego, CA. Click here for a copy of the CM Dra poster in PDF format.

44. Binary Stars AAVSO Eclipsing Binary Update. AlgolType binary stars. Astronomy101-103 Web Simulations. Simbad Astronomical Database. binary stars. http://www.dyer.vanderbilt.edu/Binary Stars.htm

AAVSO Eclipsing Binary Update Algol-Type Binary Stars Astronomy 101-103 Web Simulations Astronomy 162 Eclipsing Binary Movie ... Simbad Astronomical Database Binary Stars

45. KLUWER Academic Publishers | Magnetohydrodynamics In Binary Stars Books » Magnetohydrodynamics in binary stars. Magnetohydrodynamicsin binary stars. Add to cart. by CG Campbell Dept. of Mathematics http://www.wkap.nl/prod/b/0-7923-4606-8

Title Authors Affiliation ISBN ISSN advanced search search tips Books Magnetohydrodynamics in Binary Stars Magnetohydrodynamics in Binary Stars Add to cart by C.G. Campbell Dept. of Mathematics, University of Newcastle upon Tyne, UK Book Series: ASTROPHYSICS AND SPACE SCIENCE LIBRARY Volume 216 Magnetism in binary stars is now an area of central importance in stellar astrophysics. Magnetic fields are believed to play a fundamental role in the mass transfer process in all close binaries. After an outline of the early work in binary stars, the book introduces the fundamentals of magnetohydrodynamics and binary star theory. The main areas of MHD in binary stars are then considered, including the AM Herculis systems, intermediate polars, X-ray binary pulsars, accretion disc magnetism, and stellar and disc winds. The unifying theme is the property of magnetic fields of redistributing angular momentum, and the associated stellar spin evolution. Although this is a rapidly expanding area, the fundamental problems discussed here are likely to remain relevant for future decades. A knowledge of physics to undergraduate level is assumed. The material should be of interest to observers as well as theoreticians. Although the book is mainly aimed at research workers, parts of the text could be useful for postgraduate courses in astrophysical fluid dynamics and binary star theory.

46. KLUWER Academic Publishers | Magnetohydrodynamics In Binary Stars Books » Magnetohydrodynamics in binary stars. Magnetohydrodynamicsin binary stars. Kluwer Academic Publishers is pleased to make http://www.wkap.nl/prod/b/1-4020-0377-3

Title Authors Affiliation ISBN ISSN advanced search search tips Books Magnetohydrodynamics in Binary Stars Magnetohydrodynamics in Binary Stars Kluwer Academic Publishers is pleased to make this title available as a special Printing on Demand (PoD) edition. PoD books will be sent to you within 6-9 weeks of receipt of your order. Firm orders only!: returns cannot be accepted as PoD books are only printed on request. Add to cart by C.G. Campbell Dept. of Mathematics, University of Newcastle upon Tyne, UK Book Series: ASTROPHYSICS AND SPACE SCIENCE LIBRARY Volume 216 Magnetism in binary stars is now an area of central importance in stellar astrophysics. Magnetic fields are believed to play a fundamental role in the mass transfer process in all close binaries. After an outline of the early work in binary stars, the book introduces the fundamentals of magnetohydrodynamics and binary star theory. The main areas of MHD in binary stars are then considered, including the AM Herculis systems, intermediate polars, X-ray binary pulsars, accretion disc magnetism, and stellar and disc winds. The unifying theme is the property of magnetic fields of redistributing angular momentum, and the associated stellar spin evolution. Although this is a rapidly expanding area, the fundamental problems discussed here are likely to remain relevant for future decades. A knowledge of physics to undergraduate level is assumed. The material should be of interest to observers as well as theoreticians. Although the book is mainly aimed at research workers, parts of the text could be useful for postgraduate courses in astrophysical fluid dynamics and binary star theory.

47. Binary Stars -- From Eric Weisstein's World Of Astronomy About this site. Stars , binary stars v. binary stars, binary stars are stars whichare 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 Author: Eric W. Weisstein

48. Account Disabled binary stars Introduction and subscription information for a printed newsletterfor observers of double/binary stars. Not for the beginner. http://www.finderscope.com/objects/binaries.html

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49. Binary Stars binary stars. Test image of ADS 7071. Separation of binary is 1.5 arcseconds.Actual size Expanded view Test image of ADS 7380. Separation http://www.science.widener.edu/~schultz/sproul5.html

Binary Stars Test image of ADS 7071. Separation of binary is 1.5 arcseconds. Actual size Expanded view Test image of ADS 7380. Separation of binary is 2.2 arcseconds. Actual size Expanded view ADS 8600 R filter 0.5 seconds V filter 1 second B filter 300 seconds ADS 8489, Sep. 11.5 arcseconds, Mag. 5.9 9.0 R filter 0.4 seconds V filter 1 second B filter 300 seconds Back

50. Eclipsing Binary Stars In Globular Clusters Metropolitan Ballroom,. 71.12 Eclipsing binary stars in GlobularClusters. K. von Braun, M. Mateo (U. Michigan), L. Yan (ESO) We http://www.aas.org/publications/baas/v28n4/aas189/abs/S071012.html

Previous abstract Next abstract Session 71 - Globular Clusters. Display session, Wednesday, January 15 Metropolitan Ballroom, [71.12] Eclipsing Binary Stars in Globular Clusters K. von Braun, M. Mateo (U. Michigan), L. Yan (ESO) We present the results of our photometric monitoring project in V and I of the Galactic globular clusters M12, M15, NGC3201, and NGC6752, carried out at the Michigan-Dartmouth-MIT and Las-Campanas-Observatories over the past two years. Our aim is to identify candidates for eclipsing binary systems in these clusters for which we will then perform subsequent spectroscopic observations. The combination of the photometric and spectroscopic data can provide estimates of the masses of the individual binary components as well as the distance to the cluster. The distance estimate, which is independent of other distance scales to globular clusters, may be used to calibrate indirect distance measurement methods. In particular, the results will help establish the zero point of the RR Lyrae distance scale, and could ultimately help determine the slope of the RR Lyrae luminosity-[Fe/H] relation. The values of the masses will, in the case of an evolved binary system (with mass transfer and/or loss), provide a lower limit to the cluster's turnoff mass at its present age. For a non-evolved binary systems, we will be able to get a direct estimate of the turnoff mass. These values will be independent of cluster metallicity, interstellar reddening, as well as stellar evolution and cosmological models.

51. Session 6. Binary Stars presentation at the meeting. Session 6. binary stars. Display, Monday,January 7, 2002, 920am630pm, Exhibit Hall. 6.01 Analysis of http://www.aas.org/publications/baas/v33n4/aas199/S60.htm

AAS 199th meeting, Washington, DC, January 2002 [Previous Session] [Program listing] [Next Session] All findings are embargoed until the time of presentation at the meeting. Session 6. Binary Stars Display, Monday, January 7, 2002, 9:20am-6:30pm, Exhibit Hall Analysis of the Southern Eclipsing Variables V431 Sagittarii, V576 Centauri, BF Pavonis, and AT Aquarii R.G. Samec, M.L Stoddard, E.V. Balardelle, J.H Laird, J.O. Mattos, J.G. Miller, J. Molgaard, T.W. Brown, J.R. Weiss (Bob Jones University), Astronomy Team The RECONS Hunt for Intriguing Binaries in the Solar Neighborhood J.L. Bean (Georgia Institute of Technology), T.J. Henry, W.C. Jao, J.P. Subasavage (Georgia State University) Fundamental Parameters of the O-Type, Eclipsing Binary, HD 101213 C. Ouzts, L. R. Penny (College of Charleston) Orbits of Four Very Massive Binaries in the R136 Cluster L. R. Penny (College of Charleston), P. Massey, J. Vukovich (Lowell Observatory) Characteristics of the Population of Spectroscopic Binaries Found in the Carney-Latham Proper-Motion Survey D.W. Latham (CfA), T. Mazeh (Tel Aviv), B.W. Carney (UNC), R.P. Stefanik (CfA), J.B. Laird (Bowling Green), G. Torres (CfA), D. Goldberg (Tel Aviv), R.J. Davis (CfA), J.A. Morse (CASA) Binaries, Rotation, and Velocity Jitter in Metal-Poor Field Red Giants

52. BINARY STARS INFORMATION binary stars INFORMATION. The Orbit of 70 Ophiuchi. An eclipsing binary is a doublestar oriented so that the two stars alternately pass in front of each other. http://www.telescope.org/pparc/res5.html

PREVIOUS PAGE BINARY STARS INFORMATION The Orbit of 70 Ophiuchi By plotting the observations of a binary star over the years, it is possible to draw the orbit of one star about the other: Once the orbit is known, calculations concerning the masses of the stars can be made. This is the orbit of a faint double star in the constellation of Ophiuchus. Figure 3. An Eclipsing Binary An eclipsing binary is a double star oriented so that the two stars alternately pass in front of each other. Usually astronomers discover eclipsing binaries by noting that the brightness of a single-appearing star exhibits periodic, temporary depressions. From the shape of the resulting light curve, many details about the binary star can be deduced. Figure 4. NEXT PAGE Back to Research Contents page

53. A Triplet Of Binary Stars next up previous contents Next Electrically powered solar flares Up Researchhighlights Previous Shocking dirt between the. A triplet of binary stars. 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.

54. Papers On Binary Stars By Our Group Papers on binary stars by Our Group. Eclipsing Variable GSC 2084.0777 = ROTSE1 J174103.55+273429.1IBVS 5228 (2002); Minima of binary stars IBVS 5224 (2002); http://binaries.boulder.swri.edu/binaries/group_papers.html

Papers on Binary Stars by Our Group Photometry of OW Gem IBVS# 5347 (2002) NSV 10892 is a W UMa Eclipsing Binary IBVS# 5327 (2002) GK Dra: a delta Scuti star in a new eclipsing system discovered by Hipparcos IBVS# 5312 (2002) Light Curve Variability in XZ Canis Minoris IBVS# 5310 (2002) GSC 4153-0634 - A New Eclipsing Binary IBVS# 5305 (2002) TY Leo Is Not An Eclipsing Binary Star IBVS# 5301 (2002) GSC 00279-00321: A New W UMa Eclipsing Binary IBVS# 5299 (2002) The Contact Binary GSC 3551-1708: Light Curve Analysis IBVS# 5285 (2002) The Reddened W UMa system GSC 1851-0320 IBVS# 5271 (2002) GSC 4686 2315: A Short-period Algol IBVS# 5257 (2002) GSC 0983.1044: A Short-period RS CVn Binary IBVS# 5231 (2002) Light Elements and Light Curve of the Eclipsing Binary GSC 2605.0545 IBVS# 5229 (2002) Eclipsing Variable GSC 2084.0777 = ROTSE1 J174103.55+273429.1 IBVS# 5228 (2002) Minima of binary stars IBVS# 5224 (2002) CCD Minima of selected binary stars in 2001 IBVS# 5220 (2002) The period of LV Herculis revisited IBVS# 5201 (2001) A 100 Year Period Study of V523 Cassiopeiae: A Triple Star System?

55. RS CVn CAMPAIGN Eclipsing RS CVn binary stars. SOUTHERN STARS. HR 4980, AD Cap, VV Mon. HR 7578,RZ Eri, TY Pyx. BD 05 3578, BQ Hyi, CF Tuc. V1379 Aql, RV Lib, BH Vir. FF Aqr,AR Mon, http://capella.physics.gatech.edu/eclipses/south.html

Eclipsing RS CVn Binary Stars SOUTHERN STARS HR 4980 AD Cap VV Mon HR 7578 ... AR Mon

56. RS CVn CAMPAIGN Eclipsing RS CVn binary stars. NORTHERN STARS (V478 Lyr ER Vul). V478Lyr, V471 Tau, XY UMa. SZ Psc, V808 Tau, Epsilon UMi. UV Psc, V818 Tau,RS UMi. http://capella.physics.gatech.edu/eclipses/north3.html

Eclipsing RS CVn Binary Stars NORTHERN STARS (V478 Lyr - ER Vul) V478 Lyr V471 Tau XY UMa SZ Psc ... RW UMa

57. Binary Stars binary stars. see also Solar Astronomy, Stars. Binnendijk, Leendert. Terrell, Dirk;Murherjee, JD; and Wilson, RE binary stars A Pictorial Atlas. Krieger, 1992. http://www.ericweisstein.com/encyclopedias/books/BinaryStars.html

Binary Stars see also Solar Astronomy Stars Binnendijk, Leendert. Properties of Double Stars: A Survey of Parallaxes and Orbits. Philadelphia: University of Pennsylvania Press, 1960. 349 p. Jones, Kenneth Glyn (Ed.). Webb Society Deep-Sky Observer's Handbook, Vol. 1: Double Stars. Enslow. 166 p. $14.95. Kopal, Zdenek. Binary and Multiple Stars as Tracers of Stellar Evolution. Dordrehct, Netherlands: Reidel, 1982. $?. Kopal, Zdenek. Close Binary Systems. New York: Wiley, 1959. 558 p. Kopal, Zdenek. The Computation of Elements of Eclipsing Binary Systems. Cambridge, MA: Harvard Observatory, 1950. 181 p. Kopal, Zdenek. Dynamics of Close Binary Systems. Dordrecht, Netherlands: Reidel, 1978. 510 p. $?. Kopal, Zdenek. An Introduction to the Study of Eclipsing Variables. Cambridge, MA: Harvard University Press, 1946. 220 p. Kopal, Zdenek. Language of the Stars: A Discourse on the Theory of the Light Changes of Eclipsing Variables. Dordrecht, Netherlands: Reidel, 1979. 280 p. $63. Kopal, Zdenek.

58. ThinkQuest Library Of Entries White Stars and binary stars. They seem to be only pinpoints of light in thenight sky, but stars play an integral part in the universe. binary stars. http://library.thinkquest.org/12272/data/whitebinary.html

Welcome to the ThinkQuest Internet Challenge of Entries The web site you have requested, Lost in Space , is one of over 4000 student created entries in our Library. Before using our Library, please be sure that you have read and agreed to our To learn more about ThinkQuest. You can browse other ThinkQuest Library Entries To proceed to Lost in Space click here Back to the Previous Page The Site you have Requested ... Lost in Space click here to view this site A ThinkQuest Internet Challenge 1997 Entry Click image for the Site Languages : Site Desciption It would be difficult for anyone seeking information to be "lost in space" once they've used this web site! With sections such as an "A to Z Space Encyclopedia" and with great links out to associated subjects, the coverage of space exploration and the planets is excellent. Comets, pulsars, and other space phenomena are featured. Best of all, the graphics and animations are solidly appealing and the entire site is well-organized. Some sections of this site are under construction. Students Daniel Lemoore High School CA, United States

59. Binary Stars binary stars. The stars may be connected gravitationally (binary stars),or they may simply happen to lie nearly in the same direction. http://www.lsus.edu/nonprofit/sbas/binary.htm

BINARY STARS Binary or double stars are stars which to the naked eye appears as a single point of light, but when viewed through a telescope are found to be composed of two or more stars. The stars may be connected gravitationally (binary stars), or they may simply happen to lie nearly in the same direction. A binary star is said to be a visual binary if the components may be resolved in the telescope and their orbital motion detected by positional measurement; a spectroscopic binary if it is detected from the periodic doubling and displacement of lines in its spectrum; or a photometric binary if it is detected by the periodic variations in its magnitude (variable stars). A binary star may fall into more than one of these categories. The orbital periods range from a day or two to many centuriesthe visual binaries having periods of at least two years and the other two types normally having much shorter periods. It is estimated that more than half of the stars in our Milky Way galaxy are components of double or multiple star systems. Double and multiple stars far outnumber deep-sky objects catalogued. More than 65,000 pairs have been listed. And yet, with the exception of a few showpieces, double stars are generally ignored by serious observers. Our own sun would be considered part of a double star system, with Jupiter as its companion. Jupiter is a star that did not quite make it as a true star because it does not have enough mass to generate nuclear reactions. It does, however, emit more energy from its own slow contraction than it receives from the sun.

60. Young And Waltzing Binary Stars (ESO Press Release 22/01) For immediate release. ESO Logo. Young and Waltzing binary stars. ADONIS ObservesLowmass Eclipsing System in Orion. Summary. binary stars and stellar masses. http://www.eso.org/outreach/press-rel/pr-2001/pr-22-01.html

Information from the European Southern Observatory ESO Press Release 22/01 8 October 2001 For immediate release Young and Waltzing Binary Stars ADONIS Observes Low-mass Eclipsing System in Orion Summary A series of very detailed images of a binary system of two young stars have been combined into a movie In merely 3 days, the stars swing around each other. As seen from the earth, they pass in front of each other twice during a full revolution, producing eclipses during which their combined brightness diminishes A careful analysis of the orbital motions has now made it possible to deduce the masses of the two dancing stars . Both turn out to be about as heavy as our Sun. But while the Sun is about 4500 million years old, these two stars are still in their infancy. They are located some 1500 light-years away in the Orion star-forming region and they probably formed just 10 million years ago This is the first time such an accurate determination of the stellar masses could be achieved for a young binary system of low-mass stars . The new result provides an important piece of information for our current understanding of how young stars evolve. The observations were obtained by a team of astronomers from Italy and ESO using the ADaptive Optics Near Infrared System (ADONIS) on the 3.6-m telescope

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