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Binary Stars: more books (100)

Binary Stars: Selected Topics on Observations and Physical Processes: Lectures Held at the Astrophysics School XII. Organized by the European Astrophysics ... September, 1999. (Lecture Notes in Physics)

The Twilight River / The Tery (Dell Binary Star, no. 2.) by Gordon Eklund, F. Paul Wilson, 1979

Interacting Binary Stars by 2002-12-01

Formation of Binary Stars 2001: Proceedings of the 200th Symposium of the International Astronomical Union Held in Potsdam, Germany, 10-15 April 2000 by Germany) International Astronomical Union Symposium 2000 (Potsdam, Hans Zinnecker, et all 1999-09

Third Pacific Rim Conference on Recent Development on Binary Star Research: Proceedings of a Conference Sponsored by Chiang Mai University, Thai Astro (BDK English Tripitaka)

Light Curve Modeling of Eclipsing Binary Stars

BINARY STAR #4: LEGACY [by] Joan D. Vinge / THE JANUS EQUATION [by] Steven G. Spruill. by Joan D. Vinge, Steven Spruill, 1980-01-01

Binary Star by Helen Shay, 2003-09

Neutron Stars, Black Holes and Binary X-Ray Sources (Astrophysics and Space Science Library)

Tidal Evolution and Oscillations in Binary Stars: Third Granada Workshop on Stellar Structure: Proceedings of a Workshop Held in Granada, Spain, 26-28 (Astronomical Society of the Pacific Conference)

Magnetohydrodynamics in Binary Stars (Astrophysics and Space Science Library) by C.G. Campbell, 1997-08-31

Evolutionary Processes in Binary Stars (NATO Science Series C: Mathematical and Physical Sciences, Volume 477)

Evolutionary Processes in Interacting Binary Stars (International Astronomical Union Symposia)

Compact Stars in Binaries (International Astronomical Union Symposia)

lists with details

Eclipsing Binary Stars (Article)
ECLIPSING binary stars. A Simple Model for Computing Light Curves. INTRODUCTION.Eclipsing binary stars are just one several types of variable stars.
http://www.isc.tamu.edu/~astro/ebstar/ebstar.html

Extractions: Last updated on December 19, 1995 Eclipsing binary stars are just one several types of variable stars. These stars appear as a single point of light to an observer, but based on its brightness variation and spectroscopic observations we can say for certain that the single point of light is actually two stars in close orbit around one another. The variations in light intensity from eclipsing binary stars is caused by one star passing in front of the other relative to an observer. If we assume that the stars are spherical and that they have circular orbits, then we can easily approximate how the light varies as a function of time for eclipsing binary stars. These calculations can be performed in a relatively short computer program. A brightness versus time plot for a variable star is know as light curve . For close binary systems, time is usually expressed as
Binary Stars
binary stars By Don Ware. Looking through a telescope at the much massdo the stars have? binary stars can be of two fundamental types
http://www.astronomical.org/astbook/binary.html

Extractions: Looking through a telescope at the stars there is very little information we can gain from them. To be sure, we know what color they are and we can see that some are more luminous than others. If we use a spectrograph we can tell what elements they are made up from. From these facts alone, it is difficult to tell just how much mass they contain. By looking at pairs of stars that orbit one another we can try to answer the question, how much mass do the stars have? Binary stars can be of two fundamental types: Alberio (Visual Binary) Visual Binaries are stars that are clearly gravitational associated with one another. They orbit each other around a common center called the barycenter . Visual binaries can be seen optically through a telescope. Only a small portion of binary stars are visual binaries. In order to see a visual binary, the stars must be separated by fairly wide distances, and the orbital periods are usually very long. Optical Doubles are stars that appear to lie close together, but in fact do not, they only appear to us from our earthly observation to be close together. One of the stars in the pair is actually behind the first star and very far away. The stars of an optical double are not gravitationally bound.
Binary Stars
binary stars Planet's revolve around stars because of gravity. binary starsobey Kepler's Laws of Planetary Motion, of which there are three.
http://zebu.uoregon.edu/~js/ast222/lectures/lec05.html

Extractions: Binary Stars Planet's revolve around stars because of gravity. However, gravity is not restricted to between large and small bodies, stars can revolve around stars as well. In fact, 85% of the stars in the Milky Way galaxy are not single stars, like the Sun, but multiple star systems, binaries or triplets. If two stars orbit each other at large separations, they evolve independently and are called a wide pair . If the two stars are close enough to transfer matter by tidal forces, then they are called a close or contact pair Binary stars obey Kepler's Laws of Planetary Motion, of which there are three. It is this last law that allows us to determine the mass of the binary star system (note only the sum of the two masses).
IAU COMMISSION 42 HOMEPAGE
Organization based in Hungary that studies binary stars.
http://www.konkoly.hu:80/IAUC42/
X-ray Binary Stars - Introduction
Xray binary stars. What is a Binary Star System? X-ray Binaries. A special classof binary stars is the X-ray binaries, so-called because they emit X-rays.
http://imagine.gsfc.nasa.gov/docs/science/know_l1/binary_stars.html

Extractions: Animation of an X-ray Binary System X-ray Binary Stars Binary star systems contain two stars that orbit around their common center of mass . Many of the stars in our Galaxy are part of a binary system A special class of binary stars is the X-ray binaries, so-called because they emit X-rays . X-ray binaries are made up of a normal star and a collapsed star (a white dwarf neutron star , or black hole ). These pairs of stars produce X-rays if the stars are close enough together that material is pulled off the normal star by the gravity of the dense, collapsed star. The X-rays come from the area around the collapsed star where the material that is falling toward it is heated to very high temperatures (over a million degrees!). Show Me a Movie about X-ray Binaries!
X-ray Binary Stars
Xray binary stars. X-ray Binaries (in yellow) near the Galactic Center.If your eyes could see X-rays rather than optical light, you
http://imagine.gsfc.nasa.gov/docs/science/know_l2/binaries.html

Extractions: For Educators Show me related lesson plans X-ray Binary Stars X-ray Binaries (in yellow) near the Galactic Center If your eyes could see X-rays rather than optical light , you would see a very different and unusual sight when you looked up at the sky. You would be overwhelmed by a few hundred very bright stars , mostly concentrated towards the center of our Galaxy . Most of these stars would in fact be X-ray binaries, where a black hole or neutron star is devouring material from its companion star. A basic quest of science is to test the laws of physics under all conditions. Unexpected discoveries can lead to breakthroughs in our understanding of the laws of nature. X-ray observations of neutron stars and black holes provide a unique probe into how the Universe operates under extreme physical conditions. Mass exchange in Binary Systems
APOD Index - Stars: Binary Stars
Astronomy Picture of the Day Index Stars binary stars. Editor's choices forthe most educational Astronomy Pictures of the Day about binary stars
http://antwrp.gsfc.nasa.gov/apod/binary_stars.html

Extractions: Explanation: Our Sun is unusual in that it is alone - most stars occur in multiple or binary systems . In a binary system, the higher mass star will evolve faster and will eventually become a compact object - either a white dwarf star, a neutron star , or black hole . When the lower mass star later evolves into an expansion phase, it may be so close to the compact star that its outer atmosphere actually falls onto the compact star. Such is the case diagrammed above. Here gas from a blue giant star is shown being stripped away into an accretion disk around its compact binary companion. Gas in the accretion disk swirls around, heats up, and eventually falls onto the compact star. Extreme conditions frequently occur on the surface of the compact star as gas falls in, many times causing detectable X-rays gamma-rays , or even cataclysmic novae explosions. Studying the extreme conditions in these systems tells us about the inner properties of ordinary matter around us.
APOD: February 19, 1997 - Mizar Binary Star
Group, USNO, NRL. Explanation Mizar (sounds like My Czar ) is abinary star. In fact, most stars are binary stars. In a binary
http://antwrp.gsfc.nasa.gov/apod/ap970219.html

Extractions: Credit: J. Benson et al., NPOI Group USNO NRL Explanation Mizar (sounds like "My Czar") is a binary star. In fact, most stars are binary stars . In a binary star system , each star of the pair follows an elliptical orbital path. Mutual gravity causes the stellar companions to glide around their orbits as if tied to the ends of an elastic string passing through a balance point between them . The balance point is the system's "center of mass". Also known as zeta Ursae Majoris Mizar is the middle star in the handle of the Big Dipper and at a distance of 88 light years, was the first binary star system to be imaged telescopically . Spectroscopic observations of the Mizar system show periodic doppler shifts , revealing that both stars, Mizar A and Mizar B, are themselves binary stars! But, the companions are too close to be directly observed as separate stars, even by
Binary Stars
binary stars. Looking through a telescope at the stars there is very little informationwe can gain from them. binary stars can be of two fundamental types
http://physics.hallym.ac.kr/education/Peoria/binary.html

Extractions: Origin Looking through a telescope at the stars there is very little information we can gain from them. To be sure, we know what color they are and we can see that some are more luminous than others. If we use a spectrograph we can tell what elements they are made up from. From these facts alone, it is difficult to tell just how much mass they contain. By looking at pairs of stars that orbit one another we can try to answer the question, how much mass do the stars have? Binary stars can be of two fundamental types: Alberio (Visual Binary) Visual Binaries are stars that are clearly gravitational associated with one another. They orbit each other around a common center called the barycenter . Visual binaries can be seen optically through a telescope. Only a small portion of binary stars are visual binaries. In order to see a visual binary, the stars must be separated by fairly wide distances, and the orbital periods are usually very long. Optical Doubles are stars that appear to lie close together, but in fact do not, they only appear to us from our earthly observation to be close together. One of the stars in the pair is actually behind the first star and very far away. The stars of an optical double are not gravitationally bound. William Herschel began looking for optical doubles in 1782 with the hope that he would find a measurable parallax, by comparing a close star to the more distant star in an optical double.
IAU Symposium 200 : The Formation Of Binary Stars : Potsdam April 10-15 2000
The Formation of binary stars. 200 The Formation of binary stars was heldfrom April 10 to 15, 2000 in Potsdam (Germany), organized by the AIP.
http://www.aip.de/IAU200/

Extractions: and application for financial support: Wed, Dec 15th, 1999 Submission of poster papers: Sun, Feb 20th, 2000 Symposium takes place: Mon, Apr 10th - Sat, Apr 15th, 2000 Deadline for submission of papers: Wed, Jun 14th, 2000 Deadline for hotel registrations with guaranteed room rates: Thu, 10th Feb, 2000 Scientific organising committee: Chairpersons: H. Zinnecker, co-chair R. Mathieu, co-chair Members: P. Artymowicz A. Boss J. Bouvier C. Clarke A. Dutrey A. Ghez P. Kroupa C. Leinert S. Miyama B. Reipurth M. Simon A. Tokovinin A. Whitworth Hans Zinnecker, SOC co-chair Mark McCaughrean, LOC member Christiane Rein, secretary Phone: +49 (0)331 7499 347 Phone: +49 (0)331 7499 525 Phone +49 (0)331 7499 382 Fax: +49 (0)331 7499 267 E-mail: hzinnecker@aip.de
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 (generallyclose) 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 datethe radial velocity or "wobble" methodrequires 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. SETI THURSDAY Visit SPACE.com to explore a new SETI feature each Thursday. >>Go to SETI Thursday archive page
The Double Star Library
Workshop Spectroscopically and Spatially Resolving the Componentsof Close binary stars, Dubrovnik, Croatia; 2024 October 2003.
http://ad.usno.navy.mil/wds/dsl.html
Sixth Orbit Catalog
Sixth Catalog of Orbits of Visual binary stars. William I. Hartkopf Brian D.Mason US Naval Observatory, Washington, DC (last update 15 January 2003).
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, is one of four USNO double star catalogs recently written to CD-ROM. Copies of this CD-ROM are available upon request . Although still available on the web as well, the Fifth Catalog has been supplanted by the Sixth Catalog , so will no longer be updated. The Sixth Catalog presently includes 1,757 orbits of 1,692 systems (from a "master file" currently containing 5,025 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. Introduction Orbit grading method Description of the catalog Catalog statistics ...
BINARY STARS
English Version. Introduction. Observational Parameters. Chronometric Micrometer.Angular micrometer. Measurements New ! article about elemental statistics.
http://www.geocities.com/CapeCanaveral/Runway/8879/englishindex.html

Extractions: English Version Introduction Observational Parameters Chronometric Micrometer Angular micrometer Measurements New ! article about elemental statistics Bibliography and Links Photographs Software Download Software EFEBIN ( Bajar EFEBIN ) New !!! New version 2002 !!!, Now available EFEBIN v.2002 in english version !!!. Please, write your criticisms and suggestions to this web site, or solicit EFEBIN free , to the following address: aerusso@yahoo.com Mr. Alejandro Eduardo Russo) and I will be glad to respond Thanks for visit this page ! BACK ( Volver )
BINARY STARS
The binary stars, by Robert G. Aitken (1964). Some Bright Visual BinaryStars, by Jean Meeus, Sky and Telescope, January and February 1971.
http://www.geocities.com/CapeCanaveral/Runway/8879/englishbibliography.html

Extractions: English Version BIBLIOGRAPHY AND LINKS: books magazine web link Books: * "The Binary Stars, by Robert G. Aitken (1964). * "The Double Star Observer's Handbook, by Ronald C. Tanguay (1998). * Observing Binary and Double Stars, by Bob Argyle, Webb Society, 2002. * "Observación de estrellas dobles por aficionados, by José Luis Comellas, Agrupación Astronómica Albireo ( July 1983 ). ( in spanish ) * Astronomical Formulae for calculators, by Jean Meeus ( 1985 ). * "Astronomical Algorithms", second edition, by Jean Meeus ( 2000 ). * "Medidas Micrométricas de Estrelas Duplas em 1959-1960, by Freitas Mourau ( 1960 ). ( in portuguese ) * Index Catalogue of Visual Double Stars, 1961.0, by Hamilton M. Jeffers and Willem H. Van den Bos, with Frances M. Greeby ( I.D.S. ). Mount Hamilton, California. Publications of Lick Observatory ( 1963 ). * The Astronomical Almanac, 2001, by U.S.N.O. . * Astronomie Générale ( 1952-1953, Paris, pag. 42 ), by Danjon A. ( in french ) * Fourth Catalog of Orbits of Visual Binary Stars, by Charles E. Worley and Wulff D. Heintz, U.S.N.O. (1983).
Binary Stars
Simple explanation of binary stars in the framework of the historyof the Universe. Physical Environment binary stars.
http://www.historyoftheuniverse.com/binaries.html

Extractions: Basic Information Further Information Other Hotu Pages Questions, Answers, Comments Physical Environment ... Later This site tells the story of the history of the universe. Click Earlier and Later to follow the story. Note: Many facts have been simplified to make them easier to understand. More than half of all stars have one or more close companion stars, to which it is tied by gravity . When there are only two stars in orbit around each other they are called a binary star. When there are three or more they are called a multiple star. The closer the stars are together the faster they move. The time it takes for them to go round each other varies from days to years. Some binaries are so close that gravity pulls gas from one to the other, forming an accretion disc around the smaller star in a binary system. This releases X-ray s. A nova may also be formed by binary stars. Like this web site? Get the pocket book version with comprehensive index for only $8! Earlier 12 Billion Years ago Later ... Physical Environment Basic Information Further Information Other Hotu Pages Questions, Answers, Comments
Binary Stars
Eclipsing binary stars. by John Talbot Three dimensional Java simulationof stars that move about each other in elliptical orbits
http://www.achilles.net/~jtalbot/glossary/binary.html

Extractions: by John Talbot Three dimensional Java simulation of stars that move about each other in elliptical orbits whose orientation with respect to the observer is such that an eclipse will occur when one passes in front of the other. Your browser doesn't support Java, the above image is what you would see. Bug : move mouse off panel after changing sliders. Panel Description Light Curve Plots the light intensity variations during one orbit. The orbital phase can be set by clicking in this window (this will stop the animation if one is runnning). You can also click and while holding down the mouse button drag the mouse horizontally for more precise control over the animation speed and direction (bug: currently disabled). Earth Perspective Three dimensional animation of the binary star system. By clicking in this window you can stop and restart the animation. Blue Star Controls the luminosity, radius and mass of the blue star member of the system. Red Star Controls the luminosity, radius (in units of orbital seperation) and mass of the red star member of the system. Orbital Parameters Controls the orbit inclination, eccentricity (disabled) and the number of light samples (disabled) during one orbit.
Starfire Optical Range - Imagery (Binary Stars - More Binary Stars)
home / imagery / more binary stars binary stars in. Ursa Major, Cancer,and Delphinus. As explained in detail in The Astronomical
http://www.de.afrl.af.mil/SOR/binary2.htm

Extractions: Capella Hyakutake Comet Leonids Meteor Trails Saturn ... imagery / more binary stars Binary Stars in Ursa Major, Cancer, and Delphinus As explained in detail in The Astronomical Journal for January 2000, (Volume 119, pages 378-389), the Starfire Optical Range made extensive observations of selected binary stars, both with and without a guide star laser. The binaries are shown below, where a star observed without adaptive optics would occupy the entire field of view in each image. 10 Ursae Majoris had a separation of 0.498±0.004 arc seconds and a large magnitude difference of 1.783±0.021. phi Ursae Majoris was separated by 0.245"±0.002", with a magnitude difference of 0.277±0.026. 81 Cancri was barely resolved at 0.123"±0.001", and its magnitude difference of -0.120±0.042, indicates that the historically fainter companion is brighter at the wavelength of observation here, 0.85 microns. kappa Ursae Majoris, at a separation of 0.067"±0.001" and a magnitude difference of 0.63±0.14 magnitudes, only shows an elongation, but through detailed mathematical processing its parameters are determined. Based on this observation and other recent high-resolution measurements, a new orbit has been derived for this pair.
Starfire Optical Range - Imagery (Binary Stars - Beta Del)
home / imagery / beta del Beta Del. Download an annotated copy Fullsize GIF(33K). JPEG(25K). BetaDel (0.199 arcsec) uncompensated
http://www.de.afrl.af.mil/SOR/beta_del.htm
PROJECT CLEA: ECLIPSING BINARY STARS
Clea Home Page, ECLIPSING binary stars, Please sign our mailing list.MAC VERSION. Required Software. Click Filename to Download Or Icon
http://www.gettysburg.edu/academics/physics/clea/binstlab.html

Extractions: (Acrobat pdf format) A Description of the Lab: Purpose: To understand the observation problems involved in identifying eclipsing binary stars. To understand how to determine the period of a variable star from irregularly sampled measurements of its brightness. These two labs developed by Claud Lacy of the University of Arkansas simulate eclipsing binary stars. FindEB uses a set of 150 CCD frames, obtained by a simulated automatic telescope, of a star field containing an eclipsing binary stars. The images include the effects of astronomical "seeing" variations and atmospheric transparency variations from night to night. The object is to identify which star in the field is the eclipsing binary star. In FindPeriod, the object is to determine the orbital period of an eclipsing binary star to 6-digit accuracy from the same 150 magnitude observations used in FindEB. Both programs make use of the same data sets of measurements of magnitudes; 81 of these data sets are provided with the lab material, with provision for generating additional data sets to the user's specifications. [AVAILABLE FOR COLOR MAC ONLY]

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