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| | Binary Stars |
 | | Eclipsing binaries may also be visual or spectroscopic binaries. | | | The binary nature of the system is deduced from the periodic doppler shifts of the wavelengths of lines seen in the spectrum, as the stars move through their orbits around the center of mass. | | | Eclipsing binaries are systems in which the orbital plane is oriented exactly edgewise to the plane of the sky so that the one star passes directly in front of the other, blocking out its light during the eclipse. |
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http://astrosun2.astro.cornell.edu/academics/courses/astro201/binstar.htm
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| | Eclipsing Binaries with MONS |
| | The most interesting fact about eclipsing binaries is that all kinds of stars are found as members of binaries: from normal main sequence stars, variable stars, evolved giants and supergiants, to collapsed objects. | | | Particularly interesting are detached eclipsing binaries with low mass components (smaller than 1 solar mass) due to their paucity. | | | Analysis of components of binary stars with chromospheric activity. |
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http://astro4.ast.vill.edu/MONS/binaries.htm
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| | DIRECT Project Homepage |
| | Detached eclipsing binaries (DEBs) have the potential to establish distances to M31 and M33 with an unprecedented accuracy of better than 5% and possibly to better than 1%. | | | The DIRECT Distances to Nearby Galaxies Using Detached Eclipsing Binaries and Cepheids. | | | Check out the review paper Detached eclipsing binaries as primary distance and age indicators by Bohdan Paczynski |
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http://www.cfa.harvard.edu/~kstanek/DIRECT
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| | Binary star - Wikipedia, the free encyclopedia |
| | In the case of eclipsing binaries which are also spectroscopic binaries it is possible to make a complete solution for the specifications (mass, density, size, luminosity, and approximate shape) of both members of the system. | | | Binary stars that are simultaneously visual and spectroscopic binaries are rare, and they are a precious source of valuable information when found. | | | Conversely, spectroscopic binary stars move fast in their orbits, and this is because they are close together — usually too close to be detected as visual binaries. |
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http://en.wikipedia.org/wiki/Binary_star
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| | 68simbad.html |
| | 1986IBVS.2934....1J: JABBAR S.R., JABIR N.L., FLEYEH H.A. and MAJEED Q.S. Photoelectric observation of the eclipsing binary upsilon Herculis. | | | Your identifier (68 her) is translated to: * 68 HER ==== * 68 HER (Eclipsing binary of beta Lyr type) Coord 1950.0 = 17 15 28.60 +33 09 10.1 mb, mv = 4.63 V3 4.77 V3 Coord 2000.0 = 17 17 19.48 +33 06 00.6 sp type = B1.5Vp+... | | | 1975JBAA...85..443I: ISLES J.E. Minima of eclipsing binaries, 1973-74. |
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http://www.isc.tamu.edu/~astro/binstar/68simbad.html
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| | Eclipsing Binary Stars (Article) |
| | The variations in light intensity from eclipsing binary stars is caused by one star passing in front of the other relative to an observer. | | | The shape of the light curve for an eclipsing binary star system depends mostly on the relative brightness and size of the two stars as well as their orbital inclination as seen from Earth. | | | If your computer computes theta's that are greater than 180 degrees, then you will need to subtract them from 360 degrees to get the correct values. |
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http://www.physics.sfasu.edu/astro/ebstar/ebstar.html
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| | Binary star - Wikipedia, the free encyclopedia |
| | Unfortunately, it is impossible to obtain the complete orbit of a spectroscopic binary unless it is also a visual or an eclipsing binary, so from these objects only a determination of the joint product of mass and the sine of the angle of inclination relative to the line of sight is possible. | | | From the orbital pattern of a visual binary, or the time variation of the spectrum of a spectroscopic binary, the mass of its stars can therefore be determined. | | | Because a majority of stars exist in binary systems, binaries are particularly important to our understanding of the processes by which stars form. |
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http://en.wikipedia.org/wiki/Binary_star
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| | Astron. Astrophys. 332, 909-927 (1998) |
| | We present a spectroscopic and photometric analysis of a complex multiple system: the early-type eclipsing binary SZ Cam (O9 IV + B0.5 V) is physically bound to a third body, which itself is a close binary; this quadruple system has a visual companion, which shows evidence for duplicity as well. | | | SZ Camelopardalis - an early-type eclipsing binary embedded in a multiple system | | | Both components of this close detached binary are overluminous for their masses. |
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http://aa.springer.de/papers/8332003/2300909/small.htm
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| | Carolyn's Homepage |
| | As with the detached binary systems, the light curves of the eclipsing CVs can tell us an awful lot about the system. | | | Detached binaries are binary stars with a main-sequence or evolved secondary star orbiting a white dwarf primary. | | | Cataclysmic variables are binary stars in a close enough orbit for the late main-sequence secondary to be distorted by the gravitational pull of the white dwarf primary. |
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http://www.astro.soton.ac.uk/~csb/research.html
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| | Dr. Paul B. Etzel |
| | Stellar Astronomy: stellar properties, eclipsing binary light-curve solutions, non-degenerate interacting binaries, active chromosphere binaries, detached binaries with degenerate components. | | | Etzel, P.B. "A Simple Synthesis Method for Solving the Elements of Well-Detached Eclipsing Systems" 1981, in Photometric and Spectroscopic Binary Systems, E.B. Carling, & Z. Kopal, eds. | | | Etzel, P.B., & Olson, E.C. "New Rotational Velocities for Eclipsing Binaries, and a Comparison of Spectroscopic and Photometric Rotations" 1993, AJ, 106, 1200-1205. |
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http://mintaka.sdsu.edu/faculty/etzel
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| | Free Virtual Galaxy Project-Variable Stars |
| | Binary systems that are too close to one another may have their orbital motion detected by spectral analysis, this type of binary is known as a | | | Not only are eclipsing binaries considered variable stars (due to the apparent variation in brightness), but the eclipse data they generate stimulates very detailed studies leading to determinations of relative luminosties, masses, brightness and distance of these systems. | | | Both novae and dwarf novae are short period binary systems, that is, they are binaries with a strong mutual gravitational attraction that causes a fast rotation. |
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http://www.ccm.net/~jrsmith/variable.html
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| | Bibliography |
| | The eclipsing binary HV982 in the Large Magellanic Cloud, 1998, MNRAS, 299, 1087P N | | | KAYE, A. HD 62454 -- A New Spectroscopic Binary, 1998, IBVS, 4596, 1K | | | V. The long-period RSCVn binary HD81410 = ILHydrae, 1998, A&A, 330, 1029W |
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http://ad.usno.navy.mil/wds/dsl/bib1998.html
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| | Astronomy Labratory : Eclipsing Binaries |
| | Eclipsing binaries are variable stars, in which th light variations are caused by mutual eclipses and transits of binary star. | | | Contact binary, Semi detached binary and detached binaries. | | | Usualy contact binary has the smallest periods, and for that reason they will be the choise for observations. |
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http://www.tau.ac.il/~lab3/TELESCOPE/EB.html
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| | Catalogue: V/121 |
| | 5 (1999)> ================================================================================ ADC_Keywords: Binaries, eclipsing ; Stars, dwarfs ; Binaries, orbits ; Combined data Abstract: The catalogue contains information about 113 detached main-sequence (DMS) type detached binaries with known photometric and geometric elements. | | | V/121 Catalog of DMS-type eclipsing binaries (Svechnikov+, 1999) ================================================================================ Catalogue of orbital elements, masses and luminosities of detached main-sequence type eclipsing binaries with known photometric and spectroscopic elements orbits. | | | See also: V/42 : Close double stars (Svechnikov+, 1984) V/115 : Semidetached and semidetouched eclipsing binaries (Surkova+, 2004) V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999) V/120 : Catalog of early-type contact binaries (Bondarenko+, 1996) Byte-by-byte Description of file: catalog.dat |
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http://cdsweb.u-strasbg.fr/cgi-bin/Cat?V/121
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| | List of published papers |
| | Pribulla, T., Chochol, D., Parimucha, ©.: 1999, Period and light curve study of the eclipsing contact binary SW Lac, Contrib. | | | The main goal of this thesis was to determine basic characteristics of the components of AW UMa contact binary and find the cause of the light curve and orbital period changes. | | | Chochol, D., Pribulla, T., Teodorani, M., Errico, L., Vittone, A.A., Milano, L., Barone, F.: 1998, The RS CVn binary XY UMa as a member of a triple system, Astron. |
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http://www.ta3.sk/~pribulla/papers/papers.html
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| | Nicolaus Copernicus Astronomical Center: Marek J. Sarna: Publications |
| | The possible evolutionary scenarios for the eclipsing binary system PSR 1718--19. | | | Evolutionary scenario for short period millisecond binary pulsars. | | | Carbon abundances in semi--detached binaries: Probes into stellar physics. |
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http://www.camk.edu.pl/~sarna/1996.html
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| | CASE |
| | Eclipsing binaries hold great promise as primary distance and age indicators (Paczynski, 1996; Kruszewski & Semeniuk, 1999). | | | Attempts to use binaries for the derivation of distances and ages of globular clusters have been hampered till recently by the paucity of suitable systems. | | | In the near future we hope to obtain follow-up spectroscopic data for the already detected detached binaries. |
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http://www.camk.edu.pl/case
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| | Eclipsing Binary Research |
| | My main research is in the field of eclipsing binary stars. | | | All of these eclipsing binaries are so far away that we do not see the individual stars. | | | More than half of all stars are found to be members of orbiting pairs, called binary systems. |
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http://www.phys.appstate.edu/caton/Binaries/Binaries.htm
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| | DFS 2004 Astrophysics abstract |
| | In order to improve the determination of ages for open and globular clusters we have started a programme to observe detached eclipsing systems in such system. | | | Pinpointing isochrones in star clusters using detached eclipsing binaries | | | We describe the methods, aims and initial results of our programme and outlines the prospects for future work. |
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http://www.nbi.dk/dfs/abs2004/aa22p.html
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| | Eclipsing Binary Research and Education at Baker Observatory |
| | Among the known, longer-period, double-lined spectroscopic binaries there may be many, as yet undiscovered, eclipsing systems. | | | During the past year a Photometrics Star I thermoelectrically-cooled CCD system with a Thomson scientific-grade, metachrome-coated, 384x576 pixel CCD and fully configured computer has been mated with an eye-piece box and automated UBVRI filter wheel to provide a second complete CCD photometry system on this telescope. | | | Each student has worked at the observatory obtaining data while using the CCD camera and telescope, has learned to use IRAF on the astronomy workstation at the university and has had the opportunity to reduce and analyze the data obtained. |
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http://www.noao.edu/aura/stma/abs/gwolf.html
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| | rt.html |
| | These privileged binary systems can provide the most solid determinations of stellar | | | The agreement is impressive, as the standard deviation of the differences in the radii is 5% (as it was in the comparison with the measurement in eclipsing binaries). | | | Comparison with radii and Teffs from measurements in well-detached eclipsing binaries, as well as angular diameters and Teffs from the InfraRed Flux Method shows that for stars of solar metallicity, interpolation in the isochrones of Bertelli et al. |
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http://hebe.as.utexas.edu/cs11rt/rt.html
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| | w853.html |
| | A Photometric Analysis of the Apsidal Motion Binary System PV Cassiopeiae | | | The atmosphere of the peculiar binary system ET Andromedae | | | New masses for the O-type binary DH Cephei, and the temperatures of O-stars. |
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http://www.columbia.edu/~fms5/w853.html
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| | Effective Temperature Determination Of Eclipsing Binaries (ResearchIndex) |
| | Abstract: Effective temperatures and distances of eclipsing binaries computed through Hipparcos trigonometric parallaxes were compared with the photometric determinations. | | | The study was performed for a sample of 15 detached eclipsing binaries that can be regarded as single stars, and 9 RS... | | | The former were based on the radius, the apparent visual magnitude and the bolometric correction of the star, whereas the latter were obtained from standard calibrations using Stromgren or Johnson colour indices. |
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http://citeseer.ist.psu.edu/207041.html
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| | The Future of Massive Variability Searches (ResearchIndex) |
| | A search for detached eclipsing binaries will improve the distance scale, the value of the Hubble constant, and the age of the oldest stars. | | | 0.2: Detached Eclipsing Binaries as Primary Distance and Age Indicators - By Bohdan | | | A complete inventory of variable stars down to almost any magnitude limit will improve our understanding of the stellar evolution and the galactic structure. |
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http://citeseer.ist.psu.edu/6883.html
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| | W Ursae Majoris star Comparison Table |
| | physical object > natural object > celestial body > collection of stars > star system > binary star > close binary > eclipsing binary > W Ursae Majoris star | | | Next eclipsing binary : AS Eri Up : eclipsing binary Previous eclipsing binary : VV Cephei star |
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http://www.site.uottawa.ca:4321/astronomy/WUrsaeMajorisstar_table.html
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| | S Doradus concept from the Astronomy knowledge base |
| | physical object > natural object > celestial body > collection of stars > star system > binary star > close binary > eclipsing binary > S Doradus | | | Next eclipsing binary : Scorpius X-1 Up : eclipsing binary Previous eclipsing binary : Hercules X-1 | | | S Doradus concept from the Astronomy knowledge base |
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http://www.site.uottawa.ca:4321/astronomy/SDoradus.html
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| | Eclipsing binary - Wikipedia, the free encyclopedia |
| | An eclipsing binary star is a binary star in which the orbit plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual eclipses. | | | The light curve of an eclipsing binary is characterized by periods of practically constant light, with periodic drops in intensity. | | | In the case where the binary is also a spectroscopic binary and the parallax of the system is known, the binary is quite valuable for stellar analysis. |
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http://en.wikipedia.org/wiki/Eclipsing_binary
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| | wdsnewnotes_main.txt |
| | 00107+5453WOR 37 SX Cas, an eclipsing and spectroscopic binary, P = 36.6d. | | | A is an Algol-type eclipsing and spectroscopic binary, YZ Cas, P = 4.47d. | | | One component is a spectroscopic and eclipsing pair, V559 Cas, P = 1.58d. |
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http://ad.usno.navy.mil/wds/wdsnewnotes_main.txt
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| | Eclipsing binary - Wikipedia, the free encyclopedia |
| | The light curve of an eclipsing binary is characterized by periods of practically constant light, with periodic drops in intensity. | | | An eclipsing binary star is a binary star in which the orbit plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual eclipses. | | | Eclipsing binaries are variable stars, not because the light of the individual components vary but because of the eclipses. |
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http://en.wikipedia.org/wiki/Eclipsing_binary
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| | AS Eri Comparison Table |
| | An eclipsing binary whose secondary is close to its Roche limit. | | | Next eclipsing binary : beta Lyrae star Up : eclipsing binary Previous eclipsing binary : W Ursae Majoris star | | | Eclipsing variables whose orbital plane lies so nearly in the line of sight that eclipses, as seen from the Earth, can occur and can be detected from their light curves. |
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http://www.csi.uottawa.ca:4321/astronomy/ASEri_table.html
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