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Binary Stars:     more books (100)

The Origins, Evolution, and Destinies of Binary Stars in Clusters: An International Symposium Held at the University of Calgary, 18-23 June 1995 (Astronomical Society of the Pacific Conference Series) Zdenek Kopal's Binary Star Legacy Interacting Binary Stars (Cambridge Astrophysics) Binary and Multiple Stars as Tracers of Stellar Evolution (Astrophysics and Space Science Library) In the world of binary stars (Science for everyone) by V. M Lipunov, 1989 Binary Star #3: Dr. Scofflaw / Outerworld by Ron / Isidore Haiblum Goulart, 1979-01-01 Binary Stars as Critical Tools and Tests in Contemporary Astrophysics (IAU S240) (Proceedings of the International Astronomical Union Symposia and Colloquia) Relative Masses Of Binary Stars (1905) by Stephen Marshall Hadley, 2010-05-23 Short-Period Binary Stars: Observations, Analyses, and Results (Astrophysics and Space Science Library) Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution (International Astronomical Union Symposia) Binary Stars: A Pictorial Atlas by et al Dirk Terrell, 1992-04-01 Evolutionary Processes in Binary and Multiple Stars (Cambridge Astrophysics) by Peter Eggleton, 2006-07-24 Willing and Able (Binary Stars Vol. 3) by Jude Mason, Jenna Byrnes, 2010-07-01 Evolution of Binary and Multiple Star Systems: A Meeting in Celebration of Peter Eggleton's 60th Birthday: Proceedings Held in Bormio, Italy, 25 June - ... Society of the Pacific Conference Series)

lists with details

41. BINARY STARS
    binary stars GROUP. The binary stars group mainly concentrates on the synthesis of observable quantities for interacting binaries.  
    http://www.astro.ufl.edu/~fsgc/bstars/bstars.html
    
    Extractions: B INARY S TARS G ROUP The Binary Stars group mainly concentrates on the synthesis of observable quantities for interacting binaries. The observables are spectral energy distributions due to circumstellar gas (Dirk Terrell and R.E. Wilson), photospheric absorption line profiles for rotating stars (Jaydeep Mukherjee and R.E.Wilson), and the Stokes parameters of circumstellar polarization and limb polarization (R.E. Wilson and J.C.Liou). Dirk Terrell's hydrodynamical model has been combined with the Wilson-Liou polarization model. The ultimate goal is to understand binary star mass transfer, mass loss, and formation of particularly interesting or unusual objects. R.E. Wilson and T.J. Vaccaro are currently interested in studing long orbital period giant systems which may evolve into cataclysmic variables (dwarf + white dwarf interacting binaries) Faculty Dr. Robert Wilson Graduate Students Todd Vaccaro Department of Astronomy Home Page

42. Orbits For Inner Planets Of Binary Stars
    Orbits for Inner Planets of binary stars. What stable orbits are possible around binary stars? I poked at the problem some and found  
    http://burtleburtle.net/bob/physics/binary.html
    
    Extractions: What stable orbits are possible around binary stars? I poked at the problem some and found a couple interesting stable orbits. This was started by the question on sci.astro, is it possible for a planet to be in a stable figure-8 orbit around the two stars in a binary system? As near as I can tell, the answer is no. But there are some interesting orbits to be had. I arbitrarily chose to work with a system with circular orbits and one star 4x heavier than the other. I think any weight ratio would have yielded the same types of orbits. I suspect having slightly elliptical orbits wouldn't make too much of a difference either, but I haven't checked. Click on images to start them moving, or to stop them. Dragging changes viewpoint. It helps your CPU if you only have one running at a time. First, for reference, this is what a typical trajectory through a binary star system looks like. Stable orbits are few and far between. This is an inner planet (white) making three orbits per star system orbit. The star system is circular, with one star 4x the weight of the other. The 3::1 resonance again, except displayed once per orbit of the star system. The stars will have gone around once, the planet will have gone around twice, and they should all be in the same position every time. It's a strobe effect. The planet has been given nonnegligible mass and slight errors in the starting position, so it should wander a bit. The numbers in the corner count star system orbits (years) and show fractional energy misplaced by the simulation. See, it's stable.

43. Results With Binary Stars
    Results with binary stars. On the night of 2000 May 13, a number of binary stars were observed, as listed in Table 3.3. These were  
    http://www.mrao.cam.ac.uk/telescopes/coast/theses/rnt/node47.html
    
    Extractions: Next: Data taken on zeta Bootis Up: Observations of bright sources Previous: Timescales for exposure selection Contents On the night of 2000 May 13, a number of binary stars were observed, as listed in Table . These were used to give an indication of the imaging performance of the Lucky Exposures method for astronomical targets where an off-axis reference star is required for exposure selection and re-centring. One of the stars in the binary is used as the reference star for measurements of the Strehl ratio and relative position of the brightest speckle. After exposure selection, re-centring and co-adding, the image of the binary companion then provides a measure of the imaging PSF. The correlation between the Strehl ratios measured on one binary component with those measured on the other binary component in individual exposures can provide lower limits on both the atmospheric isoplanatism and the signal-to-noise ratio for the Strehl ratio measurements, as the dominant sources of noise (photon shot noise, stochastic detector readout noise) will not be correlated for the two stellar images. Analyses of this sort will also be presented in this section. If the detector ``pattern noise'' was strongly correlated for large distances across the short exposures this might have given a correlated error to the measured Strehl ratios for the two stars. Measurements of the summed Fourier power spectrum for the short exposure images indicate that the pattern noise should not have made a significant contribution to the Strehl ratios for these observations of

44. A Planetary Companion To The Binary Star Gamma Cephei
    a binary star system with the shortest binary period found so far and should provide an interesting case study for understanding how binary stars influence the  
    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.

45. Monoceros
    It was here that Plaskett set about studying binary stars and in 1922 this work resulted in his discovering the very massive binary star which now bears his  
    http://www.dibonsmith.com/mon_con.htm
    
    Extractions: 16 January Flanked by Orion and Canis Minor, with Gemini above and Canis Major below, the faint constellation Monoceros ("the Unicorn") is often overlooked. The stars of Monoceros are as dim as the constellation's history: only a few fourth-magnitude stars that are difficult to notice except on very clear nights.

46. Astronomy 162: Visual Binary Movies
    Visual binary stars. These movies simulate the orbit of a visual binary star pair consisting of an F0v primary and M0v secondary.  
    http://www-astronomy.mps.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

47. Lecture 8: Stellar Masses And Radii
    binary stars Apparent binary stars Chance projection of two distinct stars along the line of sight. Problems Eclipsing binary stars are very rare.  
    http://www-astronomy.mps.ohio-state.edu/~pogge/Ast162/Unit1/binaries.html
    
    Extractions: Prof. Pogge, MTWThF 11:00 Key Ideas: Types of Binary Stars: Stellar radii are measured for ~600 stars Measuring Masses Masses are measured by using the effects of gravity on objects: Examples: Binary Stars Apparent Binary Stars True Binary Stars Types of Binaries Visual Binary Spectroscopic Binary Eclipsing Binary Can separate the stars, but see the total brightness drop when they periodically eclipse each other.

48. Award#9987344 - The Formation And Destruction Of Binary Stars
    NSF Award Abstract 9987344, AWSFL008-DS3. The Formation and Destruction of binary stars. NSF Org, AST. Latest Amendment Date, June 6, 2000. Award Number, 9987344.  
    http://www.fastlane.nsf.gov/servlet/showaward?award=9987344

49. Binary Star Integrator
    Binary Star Integrator (3D). Integration Time (Binary periods). Orbit of the binary stars Mass of Star 1 (Solar masses), Mass of Star 2 (Solar masses).  
    http://janus.astro.umd.edu/orbits/3bdyB3D.html

50. Discovery Of Heaviest Binary Star Adds Weight To A Method
    Determining the mass of binary stars, using rules of gravity, will help astronomers weigh the heaviest stars in the universe.  
    http://www.space.com/scienceastronomy/astronomy/heavy_star_020130.html
    
    Extractions: One of the great ironies in astronomy is that while technology allows deeper probes of the universe and clearer pictures of its contents, basic information about stars remains hard to come by. Measuring the distance to a star is a complex undertaking. Determining diameters is incredibly difficult and has been accomplished accurately in just a handful of cases. And weighing a star? You might as well wish upon it. "For single stars, the only way to estimate a star's mass is from its luminosity," explains Philip Massey of the Lowell Observatory in Flagstaff, Arizona. Astronomers combine measurements of a star's brightness with assumptions either of how the star evolved or about the composition of its atmosphere. The two methods generate different weight estimates, however. More Stories "Evolutionary models predicted one mass, while stellar atmosphere models predicted masses that were two times smaller," Massey says. So he and some colleagues employed a well-known trick to accurately weigh a star not just any star, but one suspected of being among the heaviest known. They chose a binary star system, in which two stars orbit around one another.

51. Detecting Other Worlds: Timing Eclipsing Binary Stars Or The 'Do-Si-Do' Method
    In my last article I discussed eclipsing binary stars; a configuration of two (generally close) stars that happen to orbit each other along our line of sight  
    http://www.space.com/searchforlife/seti_doyle_worlds_011011.html
    
    Extractions: In my last article I discussed eclipsing binary stars; a configuration of two (generally close) stars that happen to orbit each other along our line of sight, thereby eclipsing each other every orbital period. The most successful way of finding planets to date—the radial velocity or "wobble" method—requires single stars since it detects the very slight offset motion of the star caused by the giant planet orbiting it. As discussed in my last article, the photometric transit method can be used to detect planets that cross two stars (the planet orbits both stars). These transits are more complex since they involve two stars orbiting each other while the planet crosses in front. The general rule for planetary stability in two-star systems is that the axis ratios should be greater than 3-to-1. This means that if two stars that orbit each other are fairly far apart, a planet could orbit one or the other at a distance of less than one-third their separation. (This is the configuration of the giant planet that orbits 16 Cygni B, the lesser bright of the 16 Cygni double star system.) On the other hand, if the two stars are very close (usually the case for eclipsing binaries) then a planet can stably orbit both, provided its orbit is at least 3 times the two stars' mutual separation. It is this latter configuration that allows the detection of outer giant planets using the eclipsing binary timing method.

52. Simulation Of Binary Star Orbits From The Hipparcos Catalog
    Please be patient while the applet loads into your browser. Once it loads, this applet will display a system of binary stars orbiting one another.  
    http://www.amherst.edu/~gsgreens/astro/Binary.html
    
    Extractions: Please be patient while the applet loads into your browser. Once it loads, this applet will display a system of binary stars orbiting one another. Select a system from the menu labelled "Binary Systems", and the simulation will begin. You'll see a white window with one red dot and one blue dot. Clicking within this window will display the coordinates in Astronomical Units (AU). In the window labelled "Position and Time Data", the elapsed time (in years) and positions (x and y in AU) for stars A and B are constantly updating. Please click on the icon (looks like an x or a /) in the upper right corner of the "stars" window before selecting a second system only one should be running at a time.

53. Binary Stars Music And Discussion
    Discussion binary stars I m pretty sure the group is called Binary Star (singular.) Anyways, Masters of the Universe is a highly inventive, beautiful group.  
    http://www.gnoosic.com/discussion/binary stars.html

54. PhysicsWeb - Binary Star Breaks Speed Record
    The researchers believe the system may be in a brief transition phase of its evolution, because the orbital periods of binary stars are thought to lengthen  
    http://physicsweb.org/article/news/6/3/16/1
    
    Extractions: 21 March 2002 New observations of a flickering astronomical X-ray source have revealed that it is the fastest-orbiting binary star system ever found. An international team led by GianLuca Israel of the Astronomical Observatory of Rome studied the pair of white dwarf stars, which orbit each other once every five minutes. Israel's team hopes the fast-moving stars could give astronomers the opportunity to detect gravitational waves predicted by Einstein's general theory of relativity. Double act In 1994, astronomers using the German ROSAT space observatory discovered a strong X-ray source in the constellation of Cancer, and noticed that its intensity fell sharply every five minutes. Binary star system are known to emit X-rays, and this prompted Israel and co-workers to study the system - known as RX J0806.3+1527 - more closely, using the Very Large Telescope in Chile and the Italian Telescopio Nazionale Galileo in the Canary Islands. The larger star in a binary system has the stronger gravitational field, which means that it draws gas and matter from its companion. Astronomers believe that the energy of this infalling material can make the 'receiving' star so hot that it emits X-rays. These X-rays are blocked from view each time the 'donor' star passes in front of its companion, leading to a sharp dip in the signal.

55. Mass Transfer In The Binary Star Algol (Beta Persei) | Astrophysics Visualizatio
    Orbiting binary stars An interactive site that allows you to adjust the various parameters (including eccentricity and angle of inclination) of a binary star  
    http://www.haydenplanetarium.org/hp/vo/ava/avapages/S1200algolbpi.html
    
    Extractions: Mass Transfer in the Binary Star Algol (Beta Persei) John M. Blondin, Marcedes T. Richards, Michael L. Malinowski (North Carolina State University) "The binary star Algol (Beta Persei) was the first eclipsing variable star ever discovered, and it's still the most famous one. Algol fades and rebrightens like clockwork every 2.87 days, and its changes are very plain to the unaided eye. The variation in its brightness is caused by one star in the system periodically blocking the other as they orbit. Astronomers have discovered that matter from one of the stars actually flows onto the other star! This supercomputer calculation shows what that matter flow might look like. FROM THE AUTHOR'S WEBSITE IN ENGLISH, PLEASE! The supercomputer calculations shown in this visualization demonstrate that, when matter flows from one star in the Algol system to the other, the stars get distorted out of their usual spherical shapes. The matter flows through a single critical point between the two stars, called the "inner Lagrangian point," and interacts with the heat and radiation from the stars to form twisted braids, loops and streamers.

56. ThinkQuest : Library : Lost In Space
    White Stars and binary stars. They seem to be only pinpoints of light in the night sky, but stars play an integral part in the universe. binary stars.  
    http://library.thinkquest.org/12272/data/whitebinary.html
    
    Extractions: Index Astronomy 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. Visit Site 1997 ThinkQuest Internet Challenge Languages English Students Daniel Lemoore High School, Lemoore, CA, United States Nicholas Lemoore High School, Lemoore, CA, United States Christopher Lemoore High School, Lemoore, CA, United States Coaches Andrea Lemoore High School, Lemoore, CA, United States Andrea Lemoore High School, Lemoore, CA, United States Andrea Lemoore High School, Lemoore, CA, United States Want to build a ThinkQuest site? The ThinkQuest site above is one of thousands of educational web sites built by students from around the world. Click here to learn how you can build a ThinkQuest site.

57. Contents
    Gravitational Waves from Coalescing Compact binary stars Gravitational wave background from nearby galaxies. Evolution of Supernova  
    http://xray.sai.msu.ru/~mystery/articles/review/node1.html
    
    Extractions: Moscow, 119899 Russia In the early 1980s, it gradually became clear that the level of understanding of stellar evolution theory, on the one hand, and the variety of astrophysical properties of stars observed in numerous space experiments, on the other hand, approached a point where in order to interpret the discovery of each new exotic source one had to invent an individual evolutionary scenario. This situation urgently required development of a general approach that would include both the complete evolutionary scenario of the joint evolution of normal and compact stars and numerical simulations of this evolution (a Scenario Machine) (Lipunov, 1982a[

58. Binary Star Data
    Eclipsing Binary Star Parameters. Data primarily from binary stars A Pictorial Atlas by Terrell, Mukherjee and Wilson. Bob Nelson s Excel file with these data.  
    http://binaries.boulder.swri.edu/atlas/
    
    Extractions: Data primarily from Binary Stars: A Pictorial Atlas by Terrell, Mukherjee and Wilson. Bob Nelson's Excel file with these data Page Star Alt ID Mode a e W P i R1(pole) R1(point) R1(side) R1(back) q R2(pole) R2(point) R2(side) R2(back) Vgam EB Type Sp Comments Photometric Reference Spectroscopic Reference Phot URL Sp. URL ID Constellation RT And EA/DW/RS "Payne-Gaposchkin, C., 1946ApJ…103..291P" RT And TW And EA/SD "ApJ 109, 95 and PASP 94, 945" TW And AB And EW/KW "Hrivnak, B.J., 1988ApJ...335..319H" "ApJ 335, 319" AB And AD And EB/DW: AD And AN And EB/DM AN And BL And EB/KE "AA 35, 327" BL And CN And EW/KW "PASP 97, 310" CN And DS And EB/DM "AK 95, 1466" DS And S Ant EW/KE: S Ant KO Aql EA/SD: "ApJ 76, 544" KO Aql OO Aql EW/DW: "ApJ 340, 458" OO Aql QY Aql EA/DS "ApSpSc 76, 111" "ApJ 103, 76" QY Aql V337 Aql EB/DM B0.5 Vp + B2V Aql V346 Aql EA/SD Aql V805 Aql EA/DM "ApJ 244, 541" Aql V889 Aql EA/DM Aql V1182 Aql EB/KE: O8 Vnn "MNRAS 250, 209" "MNRAS 225, 961" Aql RY Aqr EA/SD: "PASP 94, 945" RY Aqr ST Aqr EB/KE: "AA 35, 327" ST Aqr BW Aqr EA/DM "ApSpSc 120, 9" BW Aqr CX Aqr EA/SD "MNRAS 223, 607"

59. Binary Star
    binary star Two stars in orbit around their common center of mass and held together by their mutual gravitational pull. See binary stars, habitable planets of.  
    http://www.daviddarling.info/encyclopedia/B/binarystar.html
    
    Extractions: Two stars in orbit around their common center of mass and held together by their mutual gravitational pull. Surveys have shown that one star in every two or three is a member of a binary or multiple star system. The two components of a binary system each move in an elliptical orbit around their common center of gravity. The further apart they are, the slower they move. Their orbital periods may be measured in tens, hundreds, or even millions of years. The question of whether planets in a binary star system could conceivably support life has been widely discussed. See binary stars, habitable planets of

60. A New View Of Mizar
    Existence of such binary stars was proved by William Herschel in 1803 11 (it s worth a note that Herschel originally just wanted to apply the Galileo method  
    http://leo.astronomy.cz/mizar/article.htm
    
    Extractions: Vincent van Gogh / Starry Night on the Rhone (1888) Last year saw two interesting events in the world of double stars, both of them connected with an astronomer's old friend in the Big Dipper. While the early history of double star astronomy had to be completely rewritten after an examination of 17th century Italian manuscripts, its future at the beginning of the next millennium was briefly unveiled by the amazing precision of a new astrometric instrument, which will soon eliminate the difference between spectroscopic and visual binaries. As a bright naked-eye star in the conspicuous asterism, Mizar (Zeta UMa) was known since antiquity, of course, but who first resolved it with a telescope? Double star literature holds it was Giovanni Battista Riccioli For a long time I have been looking for a more specific reference to verify this claim. I asked historians of astronomy, even managed to check out Riccioli's two monumental surveys of the contemporary astronomy, Almagestum novum Astronomia reformata (1665), but failed to find a note about any double star at reasonable places. When I began to wonder if all that was just one of the numerous myths which, blindly copied from one book to another, change slowly but inevitably from information to noise, I quite unexpectedly chanced upon the elusive reference:

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