61. Orbits For Inner Planets Of Binary Stars Orbits for Inner Planets of binary stars. What stable orbits are possiblearound binary stars? I poked at the problem some and found http://burtleburtle.net/bob/physics/binary.html

Orbits for Inner Planets of Binary Stars 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.

62. Binary Star - Wikipedia a real double star the union of two stars that are formed together in one systemby the laws of attraction. At present, binary stars are classified into http://www.wikipedia.org/wiki/Binary_star

Main Page Recent changes Edit this page Older versions Special pages Set my user preferences My watchlist Recently updated pages Upload image files Image list Registered users Site statistics Random article Orphaned articles Orphaned images Popular articles Most wanted articles Short articles Long articles Newly created articles All pages by title Blocked IP addresses Maintenance page External book sources Printable version Talk Log in Help Binary star From Wikipedia, the free encyclopedia. A binary star system consists of two stars both orbiting around a gravitational point between them. The term "binary star" was apparently first coined by Sir William Herschel in to designate "a real double star - the union of two stars that are formed together in one system by the laws of attraction." At present, binary stars are classified into three types according to their observable properties: visual binaries spectroscopic binaries , and eclipsing binaries . Any star can belong to several of these classes, e.g. several spectroscopic binaries are also eclipsing binaries. Another three-category classification is based on the distance of the stars: detached binaries semidetached binaries and contact binaries During the past 200 years a large amount of research has been carried out on binary stars leading to some general conclusions. It is believed that at least 1/4 of all stars are at least binary systems, with as many as 10% of these systems containing more than two stars (trinary, ternary, etc.) There is a direct correlation between the period of revolution of a binary star and the

63. Reflector Book Review: Binary Stars: A Pictorial Atlas. Reflector Book Review binary stars A Pictorial Atlas. Category Scienceof Astronomy. binary stars A Pictorial Atlas by D. Terrell http://www.astroleague.org/al/bookserv/science/rev99053.html

Related Info: Astronomy Book Review Thumbnails: Biographies Instument- ation Mythology ... Book Reviews Reflector Book Review: Binary Stars: A Pictorial Atlas. Category: Science of Astronomy Binary Stars: A Pictorial Atlas by D. Terrell, J. D. Mukherjee and R.E. Wilson Krieger Publishing Co., 1992 ISBN 0-89464-041-0 $57.50, 383 8-1/2x11 pgs. hardbound When I first heard of this book I was intrigued. A primary interest of mine is double star observing. I was disappointed to find that its content was close-proximity and contact binaries. Variable star observers and astronomy students should find this book particularly valuable. Double star observers less so. The book illustrates through computer generated images how complex and diversified close binary systems can be. Over 300 such systems are displayed through different phases of their orbital revolutions They are shown as they would appear at a distance of approximately one Astronomical Unit. These illustrations are also accompanied by their appropriate light-curves and other pertinent information. Given for each pair are figures on the semi-major axis of their orbits, their eccentricity, their period, and their inclination. Other information includes the stars mean surface temperatures, mass ratio, systemic velocity, and a host of other facts, as known or deduced. I found really interesting the accompanying circle with each binary pair illustration which represents the diameter of our Sun. This circle gives us an idea of the scale of each system.

64. Simulations Of Mass Transfer In Binary Stars Hydrodynamic Simulations of Mass Transfer in Close binary stars. IntroductionAs a star exhausts its supply of hydrogen for fueling http://www.astro.psu.edu/users/mrichards/research/hydro.html

65. Binary Stars binary stars AND STELLAR MASSES. binary stars are two stars in orbit around oneanother under their mutual gravitational attraction. Optical binary stars. http://www.astro.wesleyan.edu/~anna/Astro211/0416a.html

BINARY STARS AND STELLAR MASSES Binary stars are two stars in orbit around one another under their mutual gravitational attraction. More than 50% of all stars belong to binary systems. Some binaries are members of larger groupings (triple or quadruple star systems), but many of these are dynamically unstable and will dissolve within a few rotations around the Milky Way. Classification of Binaries Binary stars are classified based on the method of their discovery: Optical Binary Stars. Not really binary stars at all - just two stars that happen to appear close together in the sky, but they are at different distances. Visual Binary Stars. Can be seen as two separate components using a telescope. Their relative position changes over the years. Astrometic Binary Stars. Only one star is seen, but its variable proper motion shows that a second, invisible, component is present. Spectroscopic Binary Stars. Discovered on the basis of their spectra. Either two sets of spectral lines are seen, or the Doppler shift of the observed lines varies periodically, indicating an invisible companion. Photometric Binary Stars, or Eclipsing Variables. Shows regular changes in the total apparent magnitude of the system, caused by the stars passing in front of each other at regular intervals.

66. Interacting Binary Stars Back to astronomy contents. Interacting binary stars. binary starsystems are as common as single stars in the universe. They are http://www.st-andrews.ac.uk/academic/physics/pandaweb/research/researchreview/as

Back to astronomy contents Interacting Binary Stars Ron Hilditch Andrew Collier Cameron Binary star systems are as common as single stars in the universe. They are of fundamental importance to astronomers because they allow stellar masses, radii and luminosities to be measured directly and can also be used as distance indicators for nearby galaxies that are resolved into individual stars. The evolution of binary stars also helps to explain a host of diverse and energetic phenomena such as novae, cataclysmic variables, symbiotic stars, x-ray binaries and some types of supernovae. More information can be found in some of our recent publications: Hilditch et al. MNRAS 291, 749, 1997; Harries et al. MNRAS 295, 386, 1998; Kaluzny et al. MNRAS 296, 347, 1998; and in the textbook An Introduction to Close Binary Stars by R W Hilditch, published by Cambridge University Press, 2001 http://star-www.st-and.ac.uk/astronomy/research.html

67. News: Decoding The Mysteries Of Binary Stars - Dr. William Bruce Weaver, MIRA Di News More news stories Decoding the Mysteries of binary stars Dr.William Bruce Weaver, MIRA Director. Chesley Bonestell's painting http://www.wardsystems.com/news.asp?11

68. JAS: Some Beautiful Binary Stars Some Beautiful binary stars. , Star, Month, Mag. Sep. PA, Colors, Remarks.1, b Cyg, Sep, 3/3.5, 34.3², 54°, Gold/sapphire, Although only optical http://www.jas.org.jo/binary.html

Some Beautiful Binary Stars Star Month Mag. Sep. P.A. Colors Remarks Cyg Sep Gold/sapphire Although only optical, a most spectacular sight; use low power Dra Sep Orange/blue Possibly optical; a real beauty h3945 CMa Feb Gold/blue One of winter's best ! CVn May Yellow/blue The famous "Cor Caroli" 872 Aur Jan Gold/blue Best seen in 15-cm (6-inch) scopes or larger And Nov Gold/blue Finest Autumn binary Boo June Yellow/red One of the closest binary (22 l.y.) 99 Her July Green/red Wide disagreement on colors Her July Red/green Primary is a variable, possibly affecting your view of companion 6 Tri Nov Yellow/blue Stunning; best seen in medium to large telescopes 70 Oph July Yellow/red Both are dwarfs; rapid period of nearly 88 years Month: Best time to observe. Mag.: Visual magnitude. Sep.: Separation (2000.0). P.A.: Position Angle (2000.0). The above table is taken from StarList 2000 by Richard Dibon-Smith. Back to JAS' Home Page Send E-mail or contact us at : The Jordanian Astronomical Society (JAS), P.O.Box 141568, Amman 11814 Jordan

69. Binary Stars //Our Business Is Helping Your Business Do Business Better! binary stars offers excellent Computer Repair, Web Hosting and GraphicDesign. Find out more by checking us out online. binary stars. http://www.binarystars.com/

Binary Stars Binary Stars welcomes you to our center for expert graphic design, e-commerce and web hosting. We have our headquarters in the neighborhood of White Lake in Oakland County Michigan. We offer a full line of services that's main purpose is to help you to achieve a formidable presence in today's largest and fastest growing market place: the Internet. Allow us to help your business shine with professional graphic design. Our graphic services range from business cards and letterheads to complete website construction and design. Please take a look at our portfolio and see. We offer services ranging from basic one-page locations to advanced e-commerce sites with shopping cart technology. This versatility is a necessity in this day and age. We also offer web hosting across the country. Customer satisfaction is always guaranteed, or labor is free*. web hosting, graphic design, ecommerce, internet, free web hosting, cheap web hosting, web design, ecommerce, anchor bar, buffalo wings, buffalo wing sauce, buffalo wing recipes, anchor bar buffalo, buffalo sauce, buffalo wings sauce, the anchor bar, anchor bar buffalo new york, anchor bar buffalo wings, buffalo wing sauce recipes, nelsonsperformance, nelsons performance, mustang flywheel, computer, services, virus, watkins flowers, watkinsflowers, graphic services inc, aci adoption consultants, image house studios, sunshine pickles, pc factory, outlook express mail, outlook, microsoft, tutorials, computer repair, network, pc, peer to peer, networking, IIS, Internet Information Services.

70. Stellar Evolution And Binary Stars Galaxy Formation Stars Stellar evolution and binary stars. StaffPeter Schröder and Robert Smith. Student James Fisher. We have http://astronomy.sussex.ac.uk/groups/stellar.html

Home Research Groups List Early Universe Galaxy Clusters ... z Stellar evolution and binary stars Staff: and Robert Smith Student: James Fisher We have recently computed a large synthetic sample of single stars, which describes the mature solar neighbourhood (d < 50 pc) and the total yield of galactic stellar mass-loss from single stars. The re-injection of stellar matter back into the galactic ISM is an important contributor to galaxy evolution, especially to its chemical evolution. A significant fraction of the mass of the galactic stellar component, however, is actually processed in binaries. To contribute to future detailed galactic models, we will study the binary component with the same techniques as applied to single stars: i.e., by computing a synthetic sample which represents the well-observed binaries of the solar neighbourhood, in order to model its evolution, and to describe and quantify the yields of the relevant mass-loss channels. On the observational side, we shall continue to study detailed properties of the stellar components in interacting binary stars, especially the effects of irradiation and the masses of the cool red components in cataclysmic binaries. Home Research Groups List Early Universe Galaxy Clusters ... z

71. Vol. 200 - The Formation Of Binary Stars Cart Checkout Sign Up for Email Updates Contact Us Request a CatalogPrivacy and Security. Vol. 200 The Formation of binary stars. http://www.astrosociety.org/online-store/scstore/p-IS200.html

Astronomical Society of the Pacific AstroShop Calendars Teacher's Library Stargazing Tools Software ... Great Bargains: Slide Sets Vol. 200 - The Formation of Binary Stars %%SoftCart.discount(IS200).DiscountDisplayProductHTML%% Price: %%SoftCart.config.currency1%% %%product(IS200).price(%%SoftCart.config.currency1%%)%% Volume S-200 Editor(s): H. Zinnecker and R. Mathieu ISBN: Published: For more information about this publication and other IAU publications, click here (a new browser window will open). ASP Home Customer Service

72. Thesis: The Mass-Ratio Distribution Of Binary Stars. Thesis about the MassRatio Distribution of Visual and Spectroscopic binary stars,by Sake J. Hogeveen, 1991. The Mass-Ratio Distribution of binary stars. http://www.astro.uu.nl/~hogeveen/thesis/

Thesis The Mass-Ratio Distribution of Binary Stars Sake J. Hogeveen, University of Amsterdam, December 20, 1991. Supervisors: Prof. dr. E.P.J. van den Heuvel and prof. dr. J. van Paradijs. The links below refer to PDF documents The complete Thesis (1.2 MB). Separately available: Table of Contents (23 kB) Introduction and Summary (37 kB) Samenvatting (summary in Dutch, 59 kB) The chapters: The mass-ratio distribution of visual binary stars , Astrophysics and Space Science, , no. 2, 1990, pp 315-342. Statistical properties of spectroscopic binary stars - As derived from The Eight Catalogue of the Orbital Elements of Spectroscopic Binary Stars , Astrophysics and Space Science, , no. 1, 1992, pp 29-46. The mass-ratio distribution of spectroscopic binary stars , Astrophysics and Space Science, , no. 2, 1992, pp 299-336. Determination of the mass-ratio distribution. I - Single-lined spectroscopic binary stars , Astrophysics and Space Science, , no. 1, 1992, pp 143-157. Determination of the mass-ratio distribution. II - Double-lined spectroscopic binary stars , Astrophysics and Space Science, , no. 2, 1992, pp 359-372.

73. MAST HUT Observations Of Variable And Binary Stars HUT Observations of Variable and binary stars. A preview of the spectrummay be viewed by clicking on the object name. The data may http://archive.stsci.edu/hut/variablebinary.html

HUT Target Search HUT Home Getting Started Search and Retrieval ... Acknowledgments HUT Observations of Variable and Binary Stars A preview of the spectrum may be viewed by clicking on the object name. The data may be retrieved by clicking on the dataid. back to the list of categories Object Ra (2000) Dec (2000) ... AO-CAS 09 Mar 1995 09:12:52 ao-cas_170 AO-CAS 16 Mar 1995 05:52:03 ao-cas_334 EG-AND 03 Mar 1995 17:16:27 eg-and_034 EG-AND 03 Mar 1995 16:53:41 eg-and_034 EG-AND 15 Mar 1995 06:29:55 eg-and_311 AX-PER 04 Mar 1995 02:35:25 ax-per_043 AX-PER 04 Mar 1995 02:27:27 ax-per_043 AX-PER 04 Mar 1995 02:35:25 ax-per_043 WX-HYI 09 Mar 1995 02:34:42 wx-hyi_163 WX-HYI 10 Mar 1995 13:29:22 wx-hyi_198 WX-HYI 12 Mar 1995 05:15:09 wx-hyi_238 EF-ERI 11 Mar 1995 15:25:38 ef-eri_224 03 Dec 1990 22:06:01 VW-HYI 04 Mar 1995 13:15:45 vw-hyi_054 VW-HYI 06 Mar 1995 13:27:34 vw-hyi_102 VW-HYI 06 Mar 1995 13:21:22 vw-hyi_102 AB-AUR 13 Mar 1995 22:58:45 ab-aur_280 ALF-ORI 12 Mar 1995 10:21:17 alf-ori_243 ALF-ORI 12 Mar 1995 10:22:59 alf-ori_243 05 Mar 1995 19:46:25 08 Dec 1990 06:05:59 U-GEM 08 Mar 1995 14:53:08 u-gem_152 U-GEM 10 Dec 1990 05:10:36 u-gem_190 YZ-CNC 04 Mar 1995 15:09:11 yz-cnc_056 YZ-CNC 06 Mar 1995 20:10:44 yz-cnc_109 10 Dec 1990 01:27:06 Z-CAM 11 Mar 1995 00:50:10 z-cam_210 Z-CAM 09 Dec 1990 13:59:44 z-cam_175 VELA-X-1 05 Mar 1995 09:05:41 vela-x-1_074 VELA-X-1 16 Mar 1995 16:32:30 vela-x-1_345 15 Mar 1995 22:44:19 EX-HYA 06 Mar 1995 03:59:34 ex-hya_092 NCEN-95 10 Mar 1995 23:59:00 ncen-95_209 UX-UMA 08 Dec 1990 19:41:23

74. Gas Disks Surrounding Binary Stars Gas Disks Surrounding binary stars. deutsch deutsch. Researchers atthe Max Planck Institute for Astrophysics propose that many close http://www.mpa-garching.mpg.de/HIGHLIGHT/2001/highlight0104_e.html

Gas Disks Surrounding Binary Stars deutsch Researchers at the Max Planck Institute for Astrophysics propose that many close binary stars are surrounded by (so far unseen) disks of gas which affect their evolution, and would explain the very high luminosity of some dwarf novae, as well as some enigmatic properties of `Black Hole binaries'. Figure 1 The image shows an `artist's impression' of a binary star consisting of a white dwarf star (white dot at the center), and a normal star orbiting around it (shown in red). They are so close that mass is pulled off the red star and flows to the white dwarf. Before settling on the white dwarf, it orbits many times around, forming a so-called accretion disk (yellow). Images like this can not be made with telescopes because the whole configuration is very small, but many indirect observations prove that objects like novae, dwarf novae and the so-called Black Hole binaries (in which the white dwarf at the center is replaced by a black hole) must look much like this. These observations also show that some gas is flowing off the disk in the form of a tenuous `wind' (shown in the picture as blue and purple haze). The crucial question is of course: if these circumbinary disks exist, can't we observe them somehow? Calculations of their predicted brightnes show that they must be quite faint, however, even if they contain a substantial amount of mass. The best chances of detection them will be at infrared wavelengths, where these binaries have only been poorly observed so far. A program of such infrared observations is under way.

75. Eclipsing Binary Stars In The OGLE-II SMC Fields Eclipsing binary stars in the OGLEII SMC fields. We present the catalogof 1459 eclipsing binary stars detected in the central 2.4 http://bulge.princeton.edu/~ogle/ogle2/ecl_smc.html

Eclipsing Binary Stars in the OGLE-II SMC fields We present the catalog of 1459 eclipsing binary stars detected in the central 2.4 square degree area of the Small Magellanic Cloud during the OGLE-II microlensing search. The sample includes objects brighter than I =20 mag with periods ranging from about 0.3 to 250 days. The average completeness of the catalog is about 80%. Statistics of the entire sample and well detached systems, suitable for distance determination, are also presented. The catalog, finding charts and BVI photometry data for all objects are available from OGLE Internet archive . See README file there for details. Users of these data are kindly requested to send us a short note. Any comments about the data and the form of their presentation are also welcome as they can improve the future releases of catalogs of variable stars detected by OGLE-II collaboration. Send your messages to this address.

76. Binary Star True binary stars are distinct from optical doubles—pairs of stars that lienearly along the same line of sight from the earth but are not physically http://www.infoplease.com/ce6/sci/A0807587.html

Trace your family history with Ancestry.com All Infoplease All Almanacs General Entertainment Sports Biographies Dictionary Encyclopedia Infoplease Home Almanacs Atlas Dictionary ... Fact Monster Kids' reference Info:Daily Fun facts Homework Center Newsletter You've got info! Help Site Map Visit related sites from: Family Education Network Encyclopedia binary star binary star 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. Biminis binary system Search Infoplease Info search tips Search Biographies Bio search tips About Us Contact Us Link to Infoplease ... Privacy

77. Eclipsing Binary Stars Observing Eclipsing binary stars. Professor Herschel Snodgrass. DepartmentPhysics. Sponsors National Science Foundation Murdock Charitable Trust. http://www.lclark.edu/~science/binary/

Observing Eclipsing Binary Stars Professor: Herschel Snodgrass Department: Physics Sponsors National Science Foundation Murdock Charitable Trust Previous Students: Colby Jurgenson Daryl MacInnes Melissa Pereira Matt Price Many of the distant points of light in the night sky are not just single stars as they appear to be but are actually two or more stars that orbit each other at close range. These component stars are often so close that their separation cannot be detected visually or even with the aid of a telescope. Some of these star systems are given away, however, by their varying brightness over the course of their orbits as one star eclipses its companion, blocking our view of its light. Our study is to monitor the brightness of several of these eclipsing binary star systems and chart their orbits and times of eclipse. We plan to continue accumulating new data to combine with old data in order to learn more about the stars' evolution and interactions. We are interested in observing changes in orbital periods as the stars are drawn together by gravity or spread apart by their obital acceleration. We also hope to observe alterations that describe phenomena such as the exchange of matter from one star to the other. If you have any questions, mail them to Herschel Snodgrass at

78. AstroRED.net - Binary Stars http://www.astrored.net/binary-stars/

79. Mass Transfer In Eccentric Binary Stars Mass Transfer in Eccentric binary stars. Dr. CA Tout, Institute ofAstronomy, cat@ast.cam.ac.uk. Since Hoyle and Crawford explained http://www.maths.cam.ac.uk/CASM/essays/abstracts/node48.html

Next: Gravitational radiation from accreting Up: Faculty of Mathematics Part Previous: Global Modes in Slowly Mass Transfer in Eccentric Binary Stars Dr. C.A. Tout, Institute of Astronomy, cat@ast.cam.ac.uk Since Hoyle and Crawford explained the Algol paradox by invoking mass transfer, much has been explained about the evolution of close binary stars in terms of Roche lobe overflow. This theory, developed in the lectures, works well for the vast majority of binary stars that have circularised and synchronized before the onset of mass transfer. There are however a few cases when mass transfer can begin before this equilibrium has been established. Examples are X-ray binaries, in which the neutron star received such a kick at formation that the system is left eccentric but still close, and close systems in dense stellar environments that encounter a third star or another binary. The current approach to the study of these systems is to use either the standard (and certainly inappropriate) Roche-lobe theory or some variant of it, such as calculating an effective Roche lobe at periastron. To study the evolution properly it is essential to know how eccentricity and asynchronicity affect mass transfer. Few attempts, such as those reported in the literature below, have been made to improve on this. In this essay you should examine the problem with a view to calculating an effective Roche-lobe radius ,which is a function not only of the separation and mass ratio of the binary but also the eccentricity

80. Astro Concepts Binary Stars binary stars. ABSTRACT. Exploration 1. The following topics are coveredduring the first Exploration binary stars and their behaviour; http://astronomy.swin.edu.au/astroconcepts/binaries.htm

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