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Binary Stars: more books (100)

Multiple Stars across the H-R Diagram: Proceedings of the ESO Workshop held in Garching, Germany, 12-15 July 2005 (ESO Astrophysics Symposia)
Close Binaries in the 21st Century: New Opportunities and Challenges
Binary Star #4: Legacy/The Janus Equation by Joan D. Vinge, Steven G. Spruill, 1980-01
Planets in Binary Star Systems (Astrophysics and Space Science Library)
Binary Stars Vol 1--Hard Lessons and Security by Jack Greene, 2010-07-01
Interacting Binaries: Saas-Fee Advanced Course 22. Lecture Notes 1992. Swiss Society for Astrophysics and Astronomy (Saas-Fee Advanced Courses) by S.N. Shore, M. Livio, et all 2010-11-02
Foreign Relations/Perfect Stranger (Binary Stars Vol 2) by Jack Greene, 2010-07-01
Interacting Binaries: Accretion, Evolution, Outcomes (AIP Conference Proceedings)
Binary and Multiple Systems of Stars (Monographs in Natural Philosophy) by Alan H. Batten, 1973-03
Binary Star Albums: One Be Lo Albums, the R.e.b.i.r.t.h., Masters of the Universe, S.o.n.o.g.r.a.m., Project F.e.t.u.s., Waterworld
Nightflyers / True Names (Binary Star #5) by George R. R. Martin, Vernor Vinge, 1981-02-01
Cataclysmic Variable Stars - How and Why they Vary (Springer Praxis Books / Space Exploration) by Coel Hellier, 2001-02-23
The Binary Stars. By Robert G. Aitken. Published by Dover. 1964 Edition by Robert G. Aitken, 1964
DYNAMICS OF PSR J0045-7319/B-STAR BINARY AND NEUTRON STAR FORMATION by DONG LAI, 1997

lists with details

Binary Star - Simple English Wikipedia, The Free Encyclopedia
A binary star is a pair of two stars which orbit around each other. For each star, the other is its companion star. Many stars are part of a system of two
http://simple.wikipedia.org/wiki/Binary_star

Extractions: Jump to: navigation search A binary star is a pair of two stars which orbit around each other. For each star, the other is its companion star . Many stars are part of a system of two or more stars. Binary stars are important in astrophysics because looking at their orbits allows scientists to find out their masses . This information can be used to learn the masses of individual stars. Binary stars are not the same as double stars , which look close together but are not connected by gravity , and may actually be far apart in space. Some binary stars can be seen as two separate stars by someone with good eyesightâ Mizar and Alcor in the handle of the Big Dipper (called "The Plough" in some countries) are an example of what is called a visual binary . Other binary stars are so close together that instruments must be used to tell them apart. One way to tell binary stars and double stars apart is to watch them for a long period of time. Over a few decades of observation, true binary stars can be seen to move around each other, but double stars always keep their same position.
Binary Star
A binary star, often called a double star, is a star system in which two stars linked by their mutual gravity orbit around a central point of mass.
http://www.scienceclarified.com/As-Bi/Binary-Star.html

Extractions: Science of Everyday Things Science in Dispute Science and Technology Binary Star forum ... As-Bi A binary star, often called a double star, is a star system in which two stars linked by their mutual gravity orbit around a central point of mass. Binary stars are quite common. A recent survey of 123 nearby Sun-like stars showed that 57 percent had one or more companions. Astrometric binary: Binary system in which only one star can be seen, but the wobble of its orbit indicates the existence of another star in orbit around it. Eclipsing binary: Mass: The quantity of matter in the star as shown by its gravitational pull on another object. Radiation: Energy in the form of waves or particles. Spectroscopic binary: A binary system that appears as one star producing two different light spectra. Spectrum: Range of individual wavelengths of radiation produced when light is broken down by the process of spectroscopy. Visual binary: Binary system in which each star can be seen directly, either through a telescope or with the naked eye. Sometimes a binary system can be detected only by using a spectroscope (a device for breaking light into its component frequencies). If a single star gives two different spectra (range of individual wavelengths of radiation), it is actually a pair of stars called a spectroscopic binary.
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

Extractions: O RBITING B INARY S TARS Astronomy 101/103 Terry Herter Description Instructions Example to try You need a JAVA enabled browser to view this simulation. A simplified derivation of the magnitude of the reflex motion of the star due to an orbiting planet can be found here 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 rightbox. 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.
Astronomy 162: Visual Binary Movies
These movies simulate the orbit of a visual binary star pair consisting of an F0v primary and M0v secondary. The orbital plane of the two is in the plane of
http://www.astronomy.ohio-state.edu/~pogge/Ast162/Movies/visbin.html

Extractions: These movies simulate the orbit of a visual binary star pair consisting of an F0v primary and M0v secondary. The orbital plane of the two is in the plane of the sky. The two stars have a mass ratio of about 3.6, appropriate for stars of this type. This movie shows the two stars in circular orbits about their center of mass (marked with the green dot). Two orbits are shown, with the orbit traced as a white line. Both stars move at a uniform speed around the center of mass, the more massive, blueish F0v star moves less as it is closer to the center-of-mass than the less massive, reddish M0v star. This movie shows the two stars in elliptical orbits about their center of mass, with an orbital eccentricity of 0.4. Watch how both stars noticeably speed up and slow down as they pass periastron (closest approach to the C-of-M) and apastron (farthest from C-of-M), respectively, thus obeying Kepler's Second Law (equal areas in equal times) the same as the planets in the Solar System. Credit: R. Pogge, OSU
Sixth Orbit Catalog
This catalog continues the series of compilations of visual binary star orbits previously published by Finsen (1934, 1938), Worley (1963), Finsen Worley
http://ad.usno.navy.mil/wds/orb6.html

Extractions: Fifth Catalog of Orbits of Visual Binary Stars . That catalog, containing orbits published through 1 January 2001, was one of four double star catalogs maintained at the USNO that were written to CD-ROM in 2001 and distributed. While that CD is now long out of print, a new version, containing catalog data as of 30 June 2006, is now in production and will be available upon request. Although still available on the web as well, the Fifth Catalog has been supplanted by the Sixth Catalog , so is no longer updated. As of 30 June 2006, the Sixth Catalog included 2,024 orbits of 1,888 systems (from a "master file" currently containing 5,693 orbits). All orbits have been graded on a 1 - 5 scale, as in earlier catalogs; the grading scheme has been modified, however, as described below. Ephemerides are included for all orbits, as are plots including all associated data in the current Washington Double Star database.
Accretion Disk Polar Jetting, Binary Star Formation And Nemesis
Brief scientific paper on accretion disk polar jetting by Max Domaschko, PhD, So. Charleston, WV, USA. Also links to a small page of hubble photographs of
http://www.aplg.com/nemesis.htm

Extractions: The Hubble Telescope has provided perplexing images of star formation . Gone is the old theory of a simple collapse of a space cloud into a solid ball. Gone also is the theory of a simple accretion disk gradually winding its way to forming star. We now see volumous jets of material mysteriously being "ejected" along the axis of the accretion disk at high velocity and extending light years out from the disk center. In addition massive quantities of material are seen as blobs at some distance from the visible outer ends of the jets. What can explain these newly observed phenomena? The star is not ejecting material but simply holding material in orbit. Outflows could be buildups of otherwise incoming particles retarded by impulses from the outer reaches of the "jetting" orbital particles. Illumination is provided by heating due to collisions between particles. Observed beading within a jet may be due clumping within the original dust cloud. The accretion disk is not a barrier to material reaching the star's core. The disk is there as a storehouse for the angular momentum imbalance of the incoming dust cloud. It varies in size, shape, and orbital plane throughout star formation as dictated by dust particles within its influence. What happens as a star system's development matures? We know from our own solar system that an accretion disk can condense into planets which orbit the star in the plane of the original accretion disk. But what happens to any polar ejectate material in a highly eccentric elliptical polar orbit? It is possible that it may also condense into a sizeable body. Depending on its size it would be another star ranging from very bright to dark or it could even be a large planet.
A Planetary Companion To The Binary Star Gamma Cephei
This planet is in a binary star system with the shortest binary period found so far and should provide an interesting case study for understanding how
http://www.as.utexas.edu/planet/gamcep.html

Extractions: A Planetary Companion to the Binary Star Gamma Cephei Precise radial velocity measurements from McDonald Observatory establish the presence of a planet orbiting the primary component of the gamma Cephei binary star system, as indicated by earlier data from the CFHT (Walker et al. 1992). This companion is the first extrasolar planet in a relatively close stellar binary system (the two stars at their closest approach are only 12 AU apart), and thus has far-reaching implications for our understanding how planets form in binary systems and for the overall frequency of planetary systems in our galaxy (since the majority of stars exist in binary or multiple systems). Artist's conception of the planet in the gamma Cephei system (click to enlarge). Note the two different shadows cast on the (hypothetical) rings of the planet by the light coming from the bright primary star, the orange K1 subgiant, and the much fainter secondary star (probably a red M-dwarf star). Radial velocity measurements of gamma Cephei showing a fraction of the binary orbit and the superimposed variation due to the planet (click to enlarge). The blue boxes are the CFHT data, while the red, green and orange symbols show the McDonald 2.7m-telescope results (the rms-values are given here in km/s). The McDonald results include 3 different data sets: 1.) the McD O2: red data-points, where telluric oxygen lines were used as the wavelength standard, 2.) McD I2: green data, a molecular iodine vapor (I2) absorption cell delivers the reference spectrum and 3.) McD cs23: orange data, the cross-dispersed Coude spectrometer using the same I2 cell.
Spaceflight Now | Breaking News | First Planet Found Orbiting Close-in Binary St
Astronomers with the McDonald Observatory Planet Search project have discovered the first planet orbiting a star in a closein binary star system.
http://www.spaceflightnow.com/news/n0210/11planet/

Extractions: Astronomers with the McDonald Observatory Planet Search project have discovered the first planet orbiting a star in a close-in binary star system. The discovery has implications for the number of possible planets in our galaxy, because unlike the Sun, most stars are in binary systems. The team announced their finding in a news conference at the American Astronomical Society's Division of Planetary Sciences meeting. Artie Hatzes (Thueringer Landessternwarte Tautenburg), Bill Cochran (UT-Austin McDonald Observatory), and colleagues found that the planet orbits the larger star of the binary system Gamma Cephei, about 45 light-years away in the constellation Cepheus. The primary star is 1.59 times as massive as the Sun. The planet is 1.76 times as massive as Jupiter. It orbits the star at about 2 Astronomical Units (A.U.), a little further than Mars's distance from the Sun. (An A.U. is the distance from Earth to the Sun.) The second, relatively small star is only 25 to 30 A.U. from the primary star about Uranus' distance from the Sun. Astronomers have found planets orbiting stars in binary systems before, but the stars in those binary systems were a hundred times farther apart than those of Gamma Cephei, Cochran said. "The stars were far enough apart to be essentially acting totally independently," he said.
Binary Star Breaks Speed Record - Physicsworld.com
New observations of a flickering astronomical Xray source have revealed that it is the fastest-orbiting binary star system ever found.
http://physicsworld.com/cws/article/news/5243

Extractions: @import url(/cws/css/screen.css); @import url(/cws/css/themes/phw.css); @import url(/cws/css/datePicker.css); Skip to the content A community website from IOP Publishing physicsworld.com ... Advertising Whole site Print edition News In depth Jobs Events Companies Products Search For maximum exposure, become a Corporate Partner. Contact our sales team Corporate Partners Mar 21, 2002 Double act The research is to appear in the journal Astronomy and Astrophysics Letters Katie Pennicott is Editor of PhysicsWeb E-mail this article to a friend A community website from IOP Publishing
Binary Star: Free Encyclopedia Articles At Questia.com Online Library
Research binary Star and other related topics by using the free encyclopedia at the Questia.com online library.
http://www.questia.com/library/encyclopedia/101232840

Extractions: Highlight the text above with the cursor. Use (ctrl + c) to copy and (ctrl + v) to paste. Mac users use (cmd + c) to copy and (cmd + v) to paste. Login Bookmark this page Link to this page Home ... Encyclopedia Index or binary system, mass-luminosity relation . Although most binary stars have distance between them, the components of W Ursae Majoris binaries are actually in contact with each other, their mutual gravity distorting their shapes into teardrops. There are binary systems in which one member is a pulsar : PSR 1913+16, for example, has an orbital period of 7 hr 45 min; in this case the other star is also a neutron star . The orbit period decreases as the system loses energy in the form of gravitational waves; used as a clock to measure the effect of the curvature of space-time on the binary's orbit, such a system confirms Einstein's theory of general relativity. Top Search the Library Books
Binary Star Modeling: Event Proceedings
The inclusion criterion for the abovelisted observation types is not that every one require a physical binary star model, but only that any combinations
http://www.ucalgary.ca/~milone/AAS97/event_proceedings.html

Extractions: 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.
Nightfall Eclipsing Binary Star Program
Interactive, userfriendly binary star program for lightcurve synthesis, animated views, data fitting and more. Can handle eccentric orbits, surface spots
http://www.hs.uni-hamburg.de/DE/Ins/Per/Wichmann/Nightfall.html

Extractions: Air Earth Fire Water ... Requirements Nightfall is an astronomy application for fun, education, and science. It can produce animated views of eclipsing binary stars, calculate synthetic lightcurves and radial velocity curves , and eventually determine the best-fit model for a given set of observational data of an eclipsing binary star system. It is, however, not able to fry your breakfast egg on your harddisk. Nightfall comes with a user guide, and a set of observational data for several eclipsing binary star systems. New: Enhanced grid of model atmospheres The screenshots show a lightcurve of the eclipsing binary star TY Boo (left), a snapshot of the animated simulation of the same star (middle), and the interactive Roche potential display (right). New: MPEG movie of OpenGL animation: output.mpg (300 kB) Nightfall is a mildly ultramundane code of baroque complexity (I like Verdi and Haendel on lazy sunday mornings - friday evenings are better with Iron Maiden and a good whisky). Nightfall is based on a physical model that takes into account the nonspherical shape of stars in close binary systems, as well as mutual irradiance of both stars, and a number of additional physical effects. Nightfall can handle a large range of binary star configurations, including overcontact (common envelope) systems, eccentric (non-circular) orbits, surface spots and asynchroneous rotation (stars rotating slower or faster than the orbital period), and the possible existence of a third star in the system ('third light').
Binary Star - Definition From The Merriam-Webster Online Dictionary
Definition of binary star from the MerriamWebster Online Dictionary with audio pronunciations, thesaurus, Word of the Day, and word games.
http://m-w.com/dictionary/binary star
Mass Transfer In Binary Star Systems - Wolfram Demonstration Project
This Demonstration shows the path of a gas particle transferred from a secondary star (S) to a more massive primary star (P) in a binary star system.
http://demonstrations.wolfram.com/MassTransferInBinaryStarSystems/

Extractions: loadFlash(522, 547, 'MassTransferInBinaryStarSystems'); This Demonstration shows the path of a gas particle transferred from a secondary star (S) to a more massive primary star (P) in a binary star system. The gas particle starts at the first Lagrange point (L1). The mass ratio is the ratio of the masses S to P. The initial velocity is shown as a blue arrow and the center of mass (C) is at the point marked +. If the gas particle is impeded by something such as an accretion disk, then its velocity must change to match the slower velocity gas in the disk. The energy lost during the impact shows as a bright spot on the edge of the accretion disk. Observing such bright spots can provide important information, such as the radius of the disk, which is not directly observable. component is the component of the initial velocity of the particle in the direction of the mass-gaining primary star. The component is the component of the initial velocity of the particle in the direction of the orbit of the mass-losing star (in this simulation, the direction is up) In a binary system, the first Lagrange point (L1) is the point of gravitational equilibrium between the two stars. When the secondary star grows so large that L1 is on its surface, gas transfers from that point to the more massive primary star. This type of system is also known as a semi-detached binary star system. The path of a particle of gas depends on its initial velocity and the friction caused by other gas particles in the transfer.
Eclipsing Binary Star, MP3 Album Music Download At EMusic
Eclipsing binary star by Astropop 3 at eMusic. MP3 album download, Brit Pop, Indie Rock.
http://www.emusic.com/album/Astropop-3-Eclipsing-binary-star-MP3-Download/109436

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