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Topic: Spectroscopic binary

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	Binary star - Wikipedia, the free encyclopedia
		Binaries are particularly crucial as one of the primary methods by which astronomers can directly measure the mass of a distant star.
		Binary stars may be found with any conceivable separation, from pairs orbiting so closely that they are practically in contact with each other, to pairs so distantly separated that their connection is indicated only by their common proper motion through space.
		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.
	en.wikipedia.org /wiki/Binary_star (1186 words)

	spectroscopic binary - Hutchinson encyclopedia article about spectroscopic binary (Site not responding. Last check: 2007-11-07)
		Binary star in which two stars are so close together that they cannot be seen separately, but their separate light spectra can be distinguished by a spectroscope.
		The first spectroscopic binary to be discovered, in 1889 by US astronomer Edward Pickering, was the brighter component of Mizar.
		The line-of-sight velocity of the brighter star, or of each star in a double-line spectroscopic binary, is measured from the Doppler shift at various stages of the orbital period.
	encyclopedia.farlex.com /spectroscopic+binary (307 words)

	Spectroscopic binary - Wikipedia, the free encyclopedia
		A spectroscopic binary star is a binary star which cannot be resolved as a visual binary, even with telescopes of the highest existing resolving power.
		In such binaries the separation between the stars is usually very small, and the orbital velocity very high.
		Since radial velocity can be measured with a spectroscope by observing the Doppler shift of the stars' spectral lines, the binaries detected in this manner are known as spectroscopic binaries.
	en.wikipedia.org /wiki/Spectroscopic_binary (340 words)

	* Spectroscopic Binary - (Astronomy): Definition (Site not responding. Last check: 2007-11-07)
		binary star that can be distinguished from a single star only through analysis of the Doppler shift of the spectral lines of one or both stars as they revolve about their common center of mass.
		SS Cyg is a double-lined, noneclipsing spectroscopic binary (sdBe, dG5) with an orbital period of 6h38m.
		A spectroscopic binary cannot be seen as two separate stars, even with the most powerful telescopes, but spectral lines from the pair show a periodic Doppler effect that indicates mutual revolution.
	en.mimi.hu /astronomy/spectroscopic_binary.html (493 words)

	Binary Stars (Site not responding. Last check: 2007-11-07)
		Spectroscopic binaries are systems in which the stars are so close together that they appear as a single star even in a telescope.
		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.
	astrosun2.astro.cornell.edu /academics/courses/astro201/binstar.htm (307 words)

	Spectroscopic binary - Encyclopedia.WorldSearch (Site not responding. Last check: 2007-11-07)
		Investigations based on the radial velocities of spectroscopic binaries and eclipsing variables (Annalen v.d.
		The orbits of the spectroscopic binaries 1 Hydrae and 75 Caneri, (Contributions from the Mount Wilson Observatory)
		The orbit of the spectroscopic binary [xi] Serpentis (Lick Observatory bulletin)
	encyclopedia.worldsearch.com /spectroscopic_binary.htm (450 words)

	Binary Stars
		Binary star systems are classified according to the manner in which they are observed: (1) Visual binary systems show two stars when observed in a telescope.
		(3) Spectroscopic binary systems again appear as a single star when viewed through a telescope, but inspection of their spectrum lines shows that the lines periodically shift back and forth (due to the Doppler effect) as the stars move in their orbits about the system's center of mass.
		Visual binaries in which the two stars are widely separated (i.e., have large orbits) ought to be easier to spot than systems where the stars are close.
	www.courses.psu.edu /astro/astro010_pjm25/binary10.html (849 words)

	Binary Stars
		Spectroscopic binaries are not detectable if we are seeing the star head on because no Doppler shifts would be present in the spectrum.
		The pattern of these light changes is called a light curve and the data for it gathered by the use of a photometer, making periodic measurements until the eclipsing binaries produce a complete orbital cycle.
		When an otherwise normal star is associated with a white dwarf companion, a type of binary called a recurrent nova, or dwarf nova may occur.
	www.astronomical.org /astbook/binary.html (1401 words)

	Project: Using Binary Stars to Measure a Cluster's Distance \| What Are Astronomers Doing?
		Binary stars are pairs of stars that orbit each other.
		Binary stars that can be identified by their spectra are called spectroscopic binary stars.
		Measuring the radial velocities of binary stars is important because it allows astronomers to determine the masses and physical separations of the two stars.
	www.mcdonaldobservatory.org /research/projects/project.php?p_id=11 (458 words)

	spectroscopic binary
		A binary star system in which the two components are so close together (see close binary), or so far from the Sun, that they cannot be resolved simply by looking at them, even through a powerful telescope.
		Their binary nature can, however, be established because of the Doppler shift of their spectral lines.
		In most cases, the components of a spectroscopic binary are so close together that each is distorted into a nonspherical shape.
	www.daviddarling.info /encyclopedia/S/specbinary.html (220 words)

	Spectroscopic binary -- Facts, Info, and Encyclopedia article (Site not responding. Last check: 2007-11-07)
		In such binaries the separation between the stars is usually very small, and the (The (usually elliptical) path described by one celestial body in its revolution about another) orbital velocity very high.
		Unless the plane of the orbit happens to be perpendicular to the line of sight, the orbital velocities will have components in the line of sight and the observed (Velocity along the line of sight toward or away from the observer) radial velocity of the system will vary periodically.
		If either a or i can be determined by other means, as in the case of (Click link for more info and facts about eclipsing binaries) eclipsing binaries, a complete solution for the orbit can be found.
	www.absoluteastronomy.com /encyclopedia/s/sp/spectroscopic_binary.htm (316 words)

	[No title] (Site not responding. Last check: 2007-11-07)
		This is the 4.85y astrometric binary of COLE et al., AJ, 103, 1357; 1992.
		A is a spectroscopic binary, B is optical.
		A is a spectroscopic binary, same period as the visual pair.
	ad.usno.navy.mil /wds/wdsnewnotes_main.txt (5089 words)

	Spectroscopic Binary Stars (Site not responding. Last check: 2007-11-07)
		In spectroscopic binary stars, we see the feature of the spectrum (spectral lines) moving back and forth in wavelength.
		This change is due to the Doppler Effect, and indicates that the sources of the radiation (the stars) are moving too, The idea of a spectroscopic binary is shown in Figures 21.4 and 21.5 on p483 of the textbook.
		Spectroscopic binaries also tend to be close-packed binaries with periods of a few days, and in some cases less than a day.
	phobos.physics.uiowa.edu /~srs/lec11/node7.html (88 words)

	spectroscopic binary concept from the Astronomy knowledge base (Site not responding. Last check: 2007-11-07)
		has definition Star whose binary nature can be detected from the periodic Doppler shifts of their spectra, owing to their varying velocities in the line of sight.
		Single-lined spectroscopic binaries have only one set of oscillating spectral lines, owing to the dimness of the secondary component.
		Spectroscopic binaries are typically of spectral type B, with almost circular orbits (whereas long-period M-type binaries have highly eccentric orbits).
	www.csi.uottawa.ca:4321 /astronomy/spectroscopicbinary.html (373 words)

	Spectroscopic binary (Site not responding. Last check: 2007-11-07)
		radial velocity can be measured with a spectroscope by observing the Doppler shift of the stars' spectral lines the binaries detected in this manner known as spectroscopic binaries.
		In some spectroscopic binaries the spectra of stars are visible and the lines are double and single.
		Determining the orbit of a spectroscopic binary done by making a long series of of the radial velocity of one or component of the binary.
	www.freeglossary.com /Spectroscopic_binary (475 words)

	Castor (star) (Site not responding. Last check: 2007-11-07)
		Castor (α Geminorum) is the fainter star of the "heavenly twins." Pollux is its partner.Since Castor and Pollux are always considered together in ancient literature, see Pollux for the history and astrologicalsignificance of the two.
		Astronomically, Castor was discovered to be a visual binary in 1719, with the magnitude of its componentsbeing 2.8 and 2.0.
		Castor has a faint companion separated from it by about 72" but having the same parallax and proper motion ; thiscompanion is also a spectroscopic binary with a period slightly less than 1 day.
	www.therfcc.org /castor-star--32095.html (155 words)

	Eclipsing Binary Stars (Site not responding. Last check: 2007-11-07)
		The majority of these stars are found in binary systems which are systems of two stars in orbit around a common center of mass.
		Other binaries are too close and far away to be seen separately but can distinguished using the doppler shift of their spectra.
		Algol the binary stars are close enough so that the eclipse one another.
	www.isc.tamu.edu /%7Eastro/binstar.html (211 words)

	Spectroscopic Binaries
		We have already seen that even if both stars cannot be seen in a binary system we may be able to infer the presence of an unseen companion by its gravitational influence on the motion of the primary star.
		Actually, most stars that are classified as binaries are not visual binaries, but instead it has been deduced that they are binaries from the spectrum.
		In many cases the spectral lines from one of the stars in a spectroscopic binary are much stronger than those from the other star.
	csep10.phys.utk.edu /astr162/lect/binaries/spectroscopic.html (614 words)

	spectroscopic binary on Encyclopedia.com (Site not responding. Last check: 2007-11-07)
		Binary births: astronomers investigate the secret lives of paired young stars.
		Solvent effects on the electronic transition energies of porhyrins in binary solvent mixtures.
		Mid-infrared microspectroscopy of difficult samples using near-field photothermal microspectroscopy: the authors discuss progress in near-field IR microspectroscopy using a photothermal probe and show how it can be...
	www.encyclopedia.com /html/X/X-spectbin.asp (368 words)

	spectroscopic binary Comparison Table (Site not responding. Last check: 2007-11-07)
		a spectroscopic binary in which periodic Doppler shift is detected in both components of the binary star each out of phase by 180 degrees
		It is a spectroscopic binary in which mass exchange is occurring.
		a spectroscopic binary in which periodic Doppler shift is detected in only one component of the binary star
	www.csi.uottawa.ca:4321 /astronomy/spectroscopicbinary_table.html (157 words)

	Spectroscopic Binary Stars (Site not responding. Last check: 2007-11-07)
		The usefulness of visual binary stars is curtailed by the need to know their distance accurately, and this is only possible if they are very close to us.
		Spectroscopic binaries are ones in which the radial velocities of one or both stars can be measured via the Doppler effect (section 3.1.2).
		6.2 and 6.3 show an example of the spectra and fitted velocities of a real spectroscopic binary with a circular orbit showing such a variation.
	www.astro.soton.ac.uk /~pac/PH112/html/notes/notes/node75.html (546 words)

	Search Results for spectroscopic binary star - Encyclopædia Britannica
		When, in a binary system (a double star whose components orbit a common centre), one component comes between the other and the Earth, an eclipse occurs and the amount of light received from both...
		This third category of binaries consists of two close stars moving in an orbit so placed in space in relation to the Earth that the light of one can at times be hidden behind the other.
		Binary stars are divided into three categories, depending on the...
	www.britannica.com /search?query=spectroscopic+binary+star (625 words)

	arihip01 Type-writer version (Site not responding. Last check: 2007-11-07)
		Pacific 94, 471) conclude that Zeta Gem is not a spectroscopic binary, since the gamma velocity of the center-of-mass of the star has been constant for 80 years.
		Such a nearly perfect alignment of Delta_mu and mu would be extremely improbable for a Delta_mu binary, but is fully consistent with a slight error in the foreshortening treatment in the GC, in which case we expect that Delta_mu is parallel or anti-parallel to mu.
		In addition to its pulsation, the star is probably a spectroscopic binary according to G. Wallerstein et al.
	www.ari.uni-heidelberg.de /arihip/arihip01.htm (13313 words)

	Spectroscopic Binary (Site not responding. Last check: 2007-11-07)
		The spectroscopic binary is defined by the absence of resolution of any star through a telescope.
		Evidence that a binary system actually exist is extrapolated from the periodic oscillations of the lines in its spectrum.
		Orbital periods for spectroscopic binary systems have been observed to range from hours up to a few months.
	www.msu.edu /~mckinn38/Binary_Stars/spectro.htm (53 words)

	www.herts.ac.uk/astro_ub/aS_ub.html (Site not responding. Last check: 2007-11-07)
		SiriusA and Sirius B are a binary star system; Sirius B being a white dwarf.
		A binary star system in which the stars are too close to one another to be observed as separate stars.
		Supernovae type I are thought to be white dwarfs in binary star systems which accrete material in a similar way to novae but, instead of there being a nova outburst, the material builds up until the resulting nuclear fusion is so powerful that its disrupts the entire star.
	www.herts.ac.uk /astro_ub/aS_ub.html (3109 words)

	About the accuracy, within which the independence of the speed of light from the movement of the source can be stated.
		There is however a large number of spectroscopic binary stars with large speeds and small or infinitesimal eccentricity, and it cannot be doubted the fact that the majority of these stars have small parallaxes and therefore will give still many smaller values for k than
		Freundlich emphasizes that the statistics of the spectroscopic binary stars exhibits a certain preference of the lines of apsides for a direction toward the sun.
		The spectroscopic binary stars with short period, thus large u, have small or infinitesimal eccentricities, while those with long periods and the visual binary stars have generally larger eccentricities.
	www.ebicom.net /~rsf1/desit-2e.htm (509 words)

	[No title] (Site not responding. Last check: 2007-11-07)
		GRIFFIN R.F. Spectroscopic binary orbits from photoelectric radial velocities.
		GRIFFIN R.F., KEENAN P.C. Spectroscopic binary orbits from photoelectric radial velocities.
		A catalogue of the observations of the mutual phenomena of the Galilean satellites of Jupiter made in 1985 during the PHEMU 85 campain.
	ftp.obs-hp.fr /www/pubs-visit/92-autres.html (194 words)

	An Astronomical Proof for the Constancy of the Speed of Light
		Now it is to be seen, that Ritz's accepted dependence of the speed of light on the movement of the source is absolutely inadmissible.
		All these dimensions are on an order with the best known spectroscopic binary stars.
		The existence of the spectroscopic binary stars and the circumstance, that...in most cases the observed radial velocity completely becomes represented by the Keplerian motion is thus a strong proof for the constancy of the speed of light.
	www.ebicom.net /~rsf1/desit-1e.htm (447 words)

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