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front of the secondary. The deeper of the two eclipses is called the primary regardless of which star is being occulted, and if a shallow second eclipse also occurs it is called the secondary eclipse. The size of the brightness drops depends on the relative brightness of the two stars, the proportion of the occulted star that is hidden, and the
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2247:", even takes this to a six-star system. In reality, some orbital ranges are impossible for dynamical reasons (the planet would be expelled from its orbit relatively quickly, being either ejected from the system altogether or transferred to a more inner or outer orbital range), whilst other orbits present serious challenges for eventual
38:
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233:), allowing him to calculate the distance to the near star. He would soon publish catalogs of about 700 double stars. By 1803, he had observed changes in the relative positions in a number of double stars over the course of 25 years, and concluded that, instead of showing parallax changes, they seemed to be
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Binaries provide the best method for astronomers to determine the mass of a distant star. The gravitational pull between them causes them to orbit around their common center of mass. From the orbital pattern of a visual binary, or the time variation of the spectrum of a spectroscopic binary, the mass
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orbiting a star. However, the requirements to perform this measurement are very exacting, due to the great difference in the mass ratio, and the typically long period of the planet's orbit. Detection of position shifts of a star is a very exacting science, and it is difficult to achieve the necessary
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Binary stars that are both visual and spectroscopic binaries are rare and are a valuable source of information when found. About 40 are known. Visual binary stars often have large true separations, with periods measured in decades to centuries; consequently, they usually have orbital speeds too small
2222:
A study of fourteen previously known planetary systems found three of these systems to be binary systems. All planets were found to be in S-type orbits around the primary star. In these three cases the secondary star was much dimmer than the primary and so was not previously detected. This discovery
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goes through an activity cycle, the outer layers of the star are subject to a magnetic torque changing the distribution of angular momentum, resulting in a change in the star's oblateness. The orbit of the stars in the binary pair is gravitationally coupled to their shape changes, so that the period
755:
detected by observing how the stars affect each other in three ways. The first is by observing extra light which the stars reflect from their companion. Second is by observing ellipsoidal light variations which are caused by deformation of the star's shape by their companions. The third method is by
3909:
Rowe, Jason F.; Borucki, William J.; Koch, David; Howell, Steve B.; Basri, Gibor; Batalha, Natalie; Brown, Timothy M.; Caldwell, Douglas; Cochran, William D.; Dunham, Edward; Dupree, Andrea K.; Fortney, Jonathan J.; Gautier, Thomas N.; Gilliland, Ronald L.; Jenkins, Jon; Latham, David W.; Lissauer,
1436:
It is also possible for widely separated binaries to lose gravitational contact with each other during their lifetime, as a result of external perturbations. The components will then move on to evolve as single stars. A close encounter between two binary systems can also result in the gravitational
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Another phenomenon observed in some Algol binaries has been monotonic period increases. This is quite distinct from the far more common observations of alternating period increases and decreases explained by the
Applegate mechanism. Monotonic period increases have been attributed to mass transfer,
811:
measurements of the movement of the visible star over a sufficiently long period of time, information about the mass of the companion and its orbital period can be determined. Even though the companion is not visible, the characteristics of the system can be determined from the observations using
791:
The visible star's position is carefully measured and detected to vary, due to the gravitational influence from its counterpart. The position of the star is repeatedly measured relative to more distant stars, and then checked for periodic shifts in position. Typically this type of measurement can
699:
of an eclipsing binary is characterized by periods of practically constant light, with periodic drops in intensity when one star passes in front of the other. The brightness may drop twice during the orbit, once when the secondary passes in front of the primary and once when the primary passes in
591:
In some spectroscopic binaries, spectral lines from both stars are visible, and the lines are alternately double and single. Such a system is known as a double-lined spectroscopic binary (often denoted "SB2"). In other systems, the spectrum of only one of the stars is seen, and the lines in the
398:
of the telescope is an important factor in the detection of visual binaries, and as better angular resolutions are applied to binary star observations, an increasing number of visual binaries will be detected. The relative brightness of the two stars is also an important factor, as glare from a
276:
If, on the contrary, two stars should really be situated very near each other, and at the same time so far insulated as not to be materially affected by the attractions of neighbouring stars, they will then compose a separate system, and remain united by the bond of their own mutual gravitation
222:
cluster, and calculated that the likelihood of finding such a close grouping of stars was about one in half a million. He concluded that the stars in these double or multiple star systems might be drawn to one another by gravitational pull, thus providing the first evidence for the existence of
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and one of the brightest stars in the nighttime sky. Astronomically, Castor was discovered to be a visual binary in 1719. Each of the components of Castor is itself a spectroscopic binary. Castor also has a faint and widely separated companion, which is also a spectroscopic binary. The
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to be measured spectroscopically. Conversely, spectroscopic binary stars move fast in their orbits because they are close together, usually too close to be detected as visual binaries. Binaries that are found to be both visual and spectroscopic thus must be relatively close to Earth.
684:
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Since about 1995, measurement of extragalactic eclipsing binaries' fundamental parameters has become possible with 8-meter class telescopes. This makes it feasible to use them to directly measure the distances to external galaxies, a process that is more accurate than using
217:
became the first person to apply the mathematics of statistics to the study of the stars, demonstrating in a paper that many more stars occur in pairs or groups than a perfectly random distribution and chance alignment could account for. He focused his investigation on the
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F0, the other (eclipsing) component is not visible. The last such eclipse occurred from 2009 to 2011, and it is hoped that the extensive observations that will likely be carried out may yield further insights into the nature of this system. Another eclipsing binary is
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form. On the other hand, other simulations suggest that the presence of a binary companion can actually improve the rate of planet formation within stable orbital zones by "stirring up" the protoplanetary disk, increasing the accretion rate of the protoplanets within.
1807:
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715:, and the relative sizes of the individual stars can be determined in terms of the radius of the orbit, by observing how quickly the brightness changes as the disc of the nearest star slides over the disc of the other star. If it is also a spectroscopic binary, the
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The orbit of a spectroscopic binary is determined by making a long series of observations of the radial velocity of one or both components of the system. The observations are plotted against time, and from the resulting curve a period is determined. If the orbit is
427:
of the secondary with respect to the primary is measured, together with the angular distance between the two stars. The time of observation is also recorded. After a sufficient number of observations are recorded over a period of time, they are plotted in
2251:
because of likely extreme variations in surface temperature during different parts of the orbit. Planets that orbit just one star in a binary system are said to have "S-type" orbits, whereas those that orbit around both stars have "P-type" or
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of −0.01. This system also underscores the fact that no search for habitable planets is complete if binaries are discounted. Alpha
Centauri A and B have an 11 AU distance at closest approach, and both should have stable habitable zones.
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Because a large proportion of stars exist in binary systems, binaries are particularly important to our understanding of the processes by which stars form. In particular, the period and masses of the binary tell us about the amount of
1285:
1339:, in which the three stars are of comparable mass, is that eventually one of the three stars will be ejected from the system and, assuming no significant further perturbations, the remaining two will form a stable binary system.
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gases from the star's outer atmosphere. These are compacted on the white dwarf's surface by its intense gravity, compressed and heated to very high temperatures as additional material is drawn in. The white dwarf consists of
1380:, thus being effectively lost to both components. Since the evolution of a star is determined by its mass, the process influences the evolution of both companions, and creates stages that cannot be attained by single stars.
1315:
rules out a single gravitating body capturing another) and the high number of binaries currently in existence, this cannot be the primary formation process. The observation of binaries consisting of stars not yet on the
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of its companion star is larger than its own. The result is that matter will transfer from one star to another through a process known as Roche lobe overflow (RLOF), either being absorbed by direct impact or through an
2127:
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
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are binary stars where one of the components fills the binary star's Roche lobe and the other does not. Gas from the surface of the Roche-lobe-filling component (donor) is transferred to the other, accreting star. The
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of the angle of inclination relative to the line of sight is possible. In the case of eclipsing binaries which are also spectroscopic binaries, it is possible to find a complete solution for the specifications (mass,
444:, and is the projection of the actual elliptical orbit of the secondary with respect to the primary on the plane of the sky. From this projected ellipse the complete elements of the orbit may be computed, where the
683:
2723:
Herschel, William (1803). "Account of the
Changes That Have Happened, during the Last Twenty-Five Years, in the Relative Situation of Double-Stars; with an Investigation of the Cause to Which They Are Owing".
366:, by measuring a deviation in a star's position caused by an unseen companion. Any binary star can belong to several of these classes; for example, several spectroscopic binaries are also eclipsing binaries.
1375:
If a star grows outside of its Roche lobe too fast for all abundant matter to be transferred to the other component, it is also possible that matter will leave the system through other
Lagrange points or as
691:
This video shows an artist's impression of an eclipsing binary star system. As the two stars orbit each other they pass in front of one another and their combined brightness, seen from a distance, decreases.
89:. Many visual binaries have long orbital periods of several centuries or millennia and therefore have orbits which are uncertain or poorly known. They may also be detected by indirect techniques, such as
1168:
Double stars are also designated by an abbreviation giving the discoverer together with an index number. α Centauri, for example, was found to be double by Father
Richaud in 1689, and so is designated
1397:: although components of a binary star form at the same time, and massive stars evolve much faster than the less massive ones, it was observed that the more massive component Algol A is still in the
1212:, are binary star systems composed of a late-type giant star and a hotter companion object. Since the nature of the companion is not well-established in all cases, it may be termed a "hot companion".
4659:
Muterspaugh; Lane; Kulkarni; Maciej
Konacki; Burke; Colavita; Shao; Hartkopf; Boss (2010). "The PHASES Differential Astrometry Data Archive. V. Candidate Substellar Companions to Binary Systems".
1222:
has been determined to be a binary star system. The secondary appears to have a higher temperature than the primary and has therefore been described as being the "hot companion" star. It may be a
1469:, causing the enormous amount of energy liberated by this process to blow the remaining gases away from the white dwarf's surface. The result is an extremely bright outburst of light, known as a
2770:, proceedings of a conference sponsored by Chiang Mai University, Thai Astronomical Society and the University of Nebraska-Lincoln held in Chiang Mai, Thailand, 26 October-1 November 1995,
229:
began observing double stars in 1779, hoping to find a near star paired with a distant star so he could measure the near star's changing position as the Earth orbited the Sun (measure its
2175:
have plenty of planets, but only one-third of binary stars do. According to theoretical simulations, even widely separated binary stars often disrupt the discs of rocky grains from which
1734:
is the semimajor axis of the second body's orbit. When the center of mass is located within the more massive body, that body appears to wobble rather than following a discernible orbit.
3966:
van
Kerkwijk, Marten H.; Rappaport, Saul A.; Breton, René P.; Justham, Stephen; Podsiadlowski, Philipp; Han, Zhanwen (2010). "Observations of Doppler Boosting in Kepler Light Curves".
780:
of the missing companion. The companion could be very dim, so that it is currently undetectable or masked by the glare of its primary, or it could be an object that emits little or no
776:
are relatively nearby stars which can be seen to wobble around a point in space, with no visible companion. The same mathematics used for ordinary binaries can be applied to infer the
1545:
1202:(Alpha Scorpii) is a red supergiant star in a binary system with a hotter blue main-sequence star Antares B. Antares B can therefore be termed a hot companion of the cool supergiant.
549:
in the light emitted from each star shifts first towards the blue, then towards the red, as each moves first towards us, and then away from us, during its motion about their common
6333:
2058:
of its orbit, with systems of short period having smaller eccentricity. Binary stars may be found with any conceivable separation, from pairs orbiting so closely that they are
2116:, this can be done only in binary and multiple star systems, making the binary stars an important class of stars. In the case of a visual binary star, after the orbit and the
277:
towards each other. This should be called a real double star; and any two stars that are thus mutually connected, form the binary sidereal system which we are now to consider.
297:. For most of the known visual binary stars one whole revolution has not been observed yet; rather, they are observed to have travelled along a curved path or a partial arc.
2265:
1509:. In this way, the relation between a star's appearance (temperature and radius) and its mass can be found, which allows for the determination of the mass of non-binaries.
719:
can also be determined, and the mass of the stars can be determined relatively easily, which means that the relative densities of the stars can be determined in this case.
2070:
of periods, with the majority of these systems orbiting with a period of about 100 years. This is supporting evidence for the theory that binary systems are formed during
3234:
Tal-Or, Lev; Faigler, Simchon; Mazeh, Tsevi (2014). "Seventy-two new non-eclipsing BEER binaries discovered in CoRoT lightcurves and confirmed by RVs from AAOmega".
1413:, and most of the mass was transferred to the other star, which is still in the main sequence. In some binaries similar to Algol, a gas flow can actually be seen.
256:, contains over 100,000 pairs of double stars, including optical doubles as well as binary stars. Orbits are known for only a few thousand of these double stars.
1039:
donor star or a white dwarf overflows the Roche lobe and falls towards the neutron star or black hole. Probably the best known example of an X-ray binary is the
4872:
Elisa V. Quintana; Fred C. Adams; Jack J. Lissauer; John E. Chambers (2007). "Terrestrial Planet
Formation around Individual Stars within Binary Star Systems".
4576:
Kraus, Adam L.; Ireland, Michael; Mann, Andrew; Huber, Daniel; Dupuy, Trent J. (2017). "The
Ruinous Influence of Close Binary Companions on Planetary Systems".
314:
is used for pairs of stars which are seen to be close together in the sky. This distinction is rarely made in languages other than
English. Double stars may be
1144:
may be used to denote the pair (for example, the binary star α Centauri AB consists of the stars α Centauri A and α Centauri B.) Additional letters, such as
1050:
for the maximum theoretical mass of a neutron star. It is therefore believed to be a black hole; it was the first object for which this was widely believed.
2183:
Detecting planets in multiple star systems introduces additional technical difficulties, which may be why they are only rarely found. Examples include the
660:
is a binary star system in which the orbital plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual
556:
In these systems, the separation between the stars is usually very small, and the orbital velocity very high. Unless the plane of the orbit happens to be
3062:
3853:
Iping, Rosina C.; Sonneborn, George; Gull, Theodore R.; Massa, Derck L.; Hillier, D. John (2005). "Detection of a Hot Binary Companion of η Carinae".
386:
star is a binary star for which the angular separation between the two components is great enough to permit them to be observed as a double star in a
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124:
If components in binary star systems are close enough, they can gravitationally distort each other's outer stellar atmospheres. In some cases, these
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companion), SS Lacertae (an eclipsing binary which stopped eclipsing), V907 Sco (an eclipsing binary which stopped, restarted, then stopped again),
592:
spectrum shift periodically towards the blue, then towards red and back again. Such stars are known as single-lined spectroscopic binaries ("SB1").
318:
or may be merely two stars that appear to be close together in the sky but have vastly different true distances from the Sun. The latter are termed
2655:
This Month in Physics History, November 27, 1783: John Michell anticipates black holes, APS News, November 2009 (Volume 18, Number 10), www.aps.org
888:
Configurations of a binary star system with a mass ratio of 3. The black lines represent the inner critical Roche equipotentials, the Roche lobes.
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81:
around each other. Binary stars in the night sky that are seen as a single object to the naked eye are often resolved as separate stars using a
3910:
Jack J.; Marcy, Geoff; Monet, David G.; Sasselov, Dimitar; Welsh, William F. (2010). "Kepler Observations of Transiting Hot Compact Objects".
3280:
2256:" orbits. It is estimated that 50–60% of binary systems are capable of supporting habitable terrestrial planets within stable orbital ranges.
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If the companion is sufficiently massive to cause an observable shift in position of the star, then its presence can be deduced. From precise
3105:
824:
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shows modulations (typically on the order of ∆P/P ~ 10) on the same time scale as the activity cycles (typically on the order of decades).
3506:
2863:"Catalogue of 500 New Nebulae, Nebulous Stars, Planetary Nebulae, and Clusters of Stars; With Remarks on the Construction of the Heavens"
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4023:
3721:
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p. 291, French astronomers, visual double stars and the double stars working group of the Société Astronomique de France, E. Soulié,
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3086:
2047:. That is, the likelihood of being in a binary or a multi-star system steadily increases as the masses of the components increase.
1047:
3763:
4960:
3298:
Asada, H.; Akasaka, T.; Kasai, M. (27 September 2004). "Inversion formula for determining parameters of an astrometric binary".
2112:
The mass of a star can be directly determined only from its gravitational attraction. Apart from the Sun and stars which act as
695:
Eclipsing binaries are variable stars, not because the light of the individual components vary but because of the eclipses. The
213:
Evidence that stars in pairs were more than just optical alignments came in 1767 when English natural philosopher and clergyman
4066:
3366:
2574:
2569:
1372:. It is not uncommon that the accretion disc is the brightest (and thus sometimes the only visible) element of a binary star.
1046:. In Cygnus X-1, the mass of the unseen companion is estimated to be about nine times that of the Sun, far exceeding the
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4406:
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3013:
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2455:. Two components of the system eclipse each other, the variation in the intensity of Algol first being recorded in 1670 by
2121:
817:
437:
17:
4938:
2547:
2150:
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and is widely separated, it is possible that the members of the pair will be designated with superscripts; an example is
3528:
Iorio, Lorenzo (2008). "On the orbital and physical parameters of the HDE 226868 / Cygnus X-1 binary system".
2620:
2338:, astronomers determined Sirius B to be 12,000 km (7,456 mi) in diameter, with a mass that is 98% of the Sun.
644:
can be determined by other means, as in the case of eclipsing binaries, a complete solution for the orbit can be found.
420:; companion). If the stars are the same brightness, the discoverer designation for the primary is customarily accepted.
6591:
6340:
5659:
2676:
2639:
1113:
350:
Binary stars are classified into four types according to the way in which they are observed: visually, by observation;
3747:
2120:
of the system has been determined, the combined mass of the two stars may be obtained by a direct application of the
912:
the stars have no major effect on each other, and essentially evolve separately. Most binaries belong to this class.
505:
1311:
between two single stars, given the very low likelihood of such an event (three objects being actually required, as
1261:
1245:
2821:
743:. Eclipsing binaries offer a direct method to gauge the distance to galaxies to an improved 5% level of accuracy.
285:
is generally restricted to pairs of stars which revolve around a common center of mass. Binary stars which can be
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3794:
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that destroys the entire star, another possible cause for runaways. An example of such an event is the supernova
253:
2407:
and the eighth-brightest star in the night time sky, which is a binary consisting of the main star with a faint
2035:
are binary or multiple, with the remaining two thirds being single stars. The overall multiplicity frequency of
518:
6345:
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5001:
4137:
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1173:
1000:
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249:
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one of the easiest observable visual binaries. The brightest member, which is the third-brightest star in the
2051:
1748:
The red cross marks the center of mass of the system. These images do not represent any specific real system.
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The Applegate mechanism explains long term orbital period variations seen in certain eclipsing binaries. As a
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6392:
6259:
3066:
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6654:
6523:
6375:
6326:
6301:
5594:
1772:(b) Two bodies with a difference in mass orbiting around a common barycenter, like the Charon–Pluto system
483:
3283:. National Center for Supercomputing Applications. University of Illinois Urbana-Champaign. Archived from
3171:
Bonanos, Alceste Z. (2006). "Eclipsing binaries: Tools for calibrating the extragalactic distance scale".
2505:
visual binary in Ursa Majoris also consists of six stars: four comprising Mizar and two comprising Alcor.
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6571:
6316:
6296:
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with each other, to pairs so distantly separated that their connection is indicated only by their common
31:
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304:
Eclipsing binary showing different phases of the smaller secondary relative to the primary star (center)
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6380:
6311:
6281:
4721:
2085:. In systems where the brightnesses are different, the fainter star is bluer if the brighter star is a
1518:
191:
2415:(an eclipsing binary which is thought to contain a black hole with a K0 star in orbit around it), and
1796:(d) Two bodies with an extreme difference in mass orbiting around a common barycenter (similar to the
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in physics, binaries give us important clues about the conditions under which the stars were formed.
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affects the apparent magnitude of the stars. Detecting binaries with these methods requires accurate
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to the line of sight, the orbital velocities have components in the line of sight, and the observed
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5404:
5039:
4712:
Daemgen, S.; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, T. (2009).
4606:
Elisa V. Quintana; Jack J. Lissauer (2007). "Terrestrial Planet Formation in Binary Star Systems".
4288:
Hoogerwerf, R.; de Bruijne, J.H.J.; de Zeeuw, P.T. (December 2000). "The Origin of Runaway Stars".
4037:
Boss, A. P. (1992). "Formation of Binary Stars". In J. Sahade; G. E. McCluskey; Yoji Kondo (eds.).
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3284:
2327:
2040:
1783:(c) Two bodies with a major difference in mass orbiting around a common barycenter (similar to the
1453:
876:
2420:
6516:
6306:
6057:
5856:
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5726:
5708:
5634:
5205:
5131:
4644:
3852:
3109:
2782:
2481:
2452:
2155:
2067:
1016:
992:
673:
476:
429:
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170:, a pair of stars that appear close to each other, have been observed since the invention of the
4116:
1655:{\displaystyle r_{1}=a\cdot {\frac {m_{2}}{m_{1}+m_{2}}}={\frac {a}{1+{\frac {m_{1}}{m_{2}}}}},}
1437:
disruption of both systems, with some of the stars being ejected at high velocities, leading to
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6447:
6219:
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6112:
6007:
5956:
5761:
5751:
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5190:
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5064:
3198:
2949:
2666:
2497:
2389:
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2365:
2361:
2335:
2299:
2283:
2168:
2129:
2082:
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1312:
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has discovered examples of eclipsing binary stars where the secondary is the hotter component.
1216:
1152:, etc., may be used for systems with more than two stars. In cases where the binary star has a
1040:
1036:
1028:
1024:
761:
752:
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601:
359:
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Over the years, many more double stars have been catalogued and measured. As of June 2017, the
46:
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3514:
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discovered the companion (Sirius B; the visible star is Sirius A). In 1915 astronomers at the
2159:
Schematic of a binary star system with one planet on an S-type orbit and one on a P-type orbit
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6708:
6581:
6321:
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6286:
6276:
6204:
5992:
5158:
3760:
2537:
2096:
1784:
1426:
1308:
1020:
996:
705:
105:). If a binary star happens to orbit in a plane along our line of sight, its components will
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4943:
4744:
4713:
4517:
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Another classification is based on the distance between the stars, relative to their sizes:
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6167:
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3619:
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3143:
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2167:, such systems are comparatively rare compared to single star systems. Observations by the
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609:
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of the ellipse and the orientation of the major axis with reference to the line of sight.
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each other in binary systems. The first orbit of a binary star was computed in 1827, when
8:
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through space. Among gravitationally bound binary star systems, there exists a so-called
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832:
708:) of the stars. Typically the occultation of the hotter star causes the primary eclipse.
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4787:
4682:
4629:
4589:
4456:
4390:
4311:
4237:
4163:
3989:
3933:
3876:
3831:
3808:– see essential notes: "Hot companion to Antares at 2.9arcsec; estimated period: 678yr."
3660:
3623:
3475:
3413:
3321:
3194:
3147:
3090:
2878:
6759:
6747:
6644:
6457:
6418:
6370:
6355:
6269:
6209:
6132:
6042:
6012:
6002:
5946:
5868:
5559:
5195:
4994:
4907:
4881:
4854:
4826:
4756:
4730:
4694:
4690:
4668:
4615:
4575:
4529:
4503:
4460:
4434:
4376:
4323:
4297:
4251:
4223:
4001:
3975:
3945:
3941:
3919:
3888:
3862:
3672:
3563:
3537:
3487:
3461:
3427:
3399:
3333:
3307:
3261:
3243:
3216:
3180:
2892:
2749:
2741:
2627:, Giovanni Battista Riccioli, Bononiae: Ex typographia haeredis Victorij Benatij, 1651.
2485:
2323:
2311:
2164:
2113:
2105:
2078:
2036:
1336:
1092:
941:
701:
585:
545:
on its emitted light. In these cases, the binary consists of a pair of stars where the
395:
286:
195:
4957:
2451:
is the most noted ternary (long thought to be a binary), located in the constellation
2275:
The large distance between the components, as well as their difference in color, make
6408:
5833:
5806:
5786:
5586:
5370:
5358:
5185:
5165:
5119:
5101:
5069:
4533:
4464:
4402:
4255:
4190:
4171:
4096:
4042:
3997:
3949:
3892:
3743:
3701:
3676:
3422:
3385:
3265:
3009:
2978:
2926:
2753:
2703:
2672:
2532:
2472:), which was probably given due to its peculiar behavior. Another visible ternary is
1458:
1394:
1352:
1153:
953:
827:
740:
534:
156:
132:
5893:
4911:
4858:
4698:
4070:
4005:
3431:
3370:
3337:
3220:
2223:
resulted in a recalculation of parameters for both the planet and the primary star.
1332:
is an acceptable explanation for the formation of a binary or multiple star system.
626:. However, the product of the semi-major axis and the sine of the inclination (i.e.
6735:
6618:
6576:
6236:
6189:
6139:
6127:
6105:
6100:
6027:
5987:
5934:
5716:
5639:
5614:
5508:
5429:
5153:
5114:
4899:
4844:
4760:
4748:
4686:
4521:
4452:
4394:
4327:
4315:
4241:
4167:
3993:
3937:
3880:
3835:
3664:
3627:
3567:
3555:
3491:
3479:
3417:
3325:
3257:
3253:
3208:
3151:
2882:
2733:
2496:
is a sextuple star system, which is the second-brightest star in the constellation
2341:
2319:
1514:
1369:
1070:
1027:
according to the mass of the donor star. High-mass X-ray binaries contain a young,
772:
Astronomers have discovered some stars that seemingly orbit around an empty space.
736:
716:
269:
242:
226:
148:
4752:
3697:
3691:
3005:
2999:
2805:, Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf, Astrometry Department,
6423:
6226:
6095:
5939:
5910:
5851:
5846:
5721:
5449:
5414:
5348:
5294:
5289:
5234:
5044:
4964:
4525:
4371:
Fender, R. (2002). "Relativistic Outflows from X-ray Binaries ('Microquasars')".
4062:
3790:
2974:
2964:
2922:
2916:
2825:
2802:
2795:
2699:
2693:
2643:
2624:
2558:
2502:
2460:
2357:
2226:
1368:. The mathematical point through which this transfer happens is called the first
1325:
957:
923:
dominates the evolution of the system. In many cases, the inflowing gas forms an
813:
746:
724:
616:
561:
445:
399:
bright star may make it difficult to detect the presence of a fainter component.
199:
4150:
Boyle, C.B. (1984). "Mass transfer and accretion in close binaries – A review".
564:
of the system varies periodically. Since radial velocity can be measured with a
238:
6634:
6485:
6251:
6090:
5917:
5888:
5863:
5796:
5485:
5353:
5239:
5141:
5031:
5021:
4849:
4812:
2563:
2473:
2071:
2059:
1700:
1462:
1365:
1321:
1233:
1205:
1074:
1058:
1008:
968:
949:
932:
924:
569:
550:
542:
424:
334:
290:
4958:
Selected visual double stars and their relative position as a function of time
4210:
Chen, Z; A. Frank; E. G. Blackman; J. Nordhaus; J. Carroll-Nellenback (2017).
3559:
3483:
3212:
2768:
The Third Pacific Rim Conference on Recent Development of Binary Star Research
2310:
is another binary and the brightest star in the night time sky, with a visual
1035:, while low-mass X-ray binaries are semidetached binaries in which gas from a
1007:, where the compact object is a white dwarf, are examples of such systems. In
410:
In some publications (especially older ones), a faint secondary is called the
37:
6781:
6690:
6675:
6437:
6231:
6194:
6162:
6037:
5746:
5569:
5540:
5518:
5136:
5109:
5086:
4987:
3767:
3132:"Eclipsing binary solutions in physical units and direct distance estimation"
2614:
2527:
2493:
2444:
2396:
2392:
2303:
2280:
2090:
2063:
1831:
1710:
is the semimajor axis of the first body's orbit around the center of mass or
1406:
1398:
1389:
1348:
1317:
1157:
920:
909:
797:
573:
557:
546:
382:
375:
355:
127:
4811:
Schlaufman, Kevin C.; Thompson, Ian B.; Casey, Andrew R. (5 November 2018).
4398:
3329:
2636:
1461:
and so is largely unresponsive to heat, while the accreted hydrogen is not.
908:
of the star itself is larger than that of the other component. While on the
711:
An eclipsing binary's period of orbit may be determined from a study of its
6649:
6586:
6566:
6561:
6497:
6172:
6122:
6117:
6017:
5900:
5883:
5841:
5811:
5801:
5736:
5619:
5564:
5545:
5525:
5503:
5495:
5338:
5331:
5170:
5091:
5074:
4246:
4211:
2887:
2737:
2412:
2216:
2204:
2192:
2176:
2044:
1828:
1760:(a) Two bodies of similar mass orbiting around a common center of mass, or
1438:
1377:
1032:
1012:
988:
980:
936:
is a type of binary star in which both components of the binary fill their
785:
668:
of the system is known, the binary is quite valuable for stellar analysis.
565:
351:
214:
90:
4932:
3724:. Lawrence Hall of Science at the University of California. Archived from
636:) may be determined directly in linear units (e.g. kilometres). If either
6670:
6608:
6542:
6413:
6077:
6067:
6047:
6022:
5951:
5873:
5629:
5604:
5599:
5513:
5473:
5434:
5399:
5382:
5377:
5049:
4886:
4508:
4381:
4302:
3867:
3466:
3312:
3185:
2521:
2515:
2408:
2404:
2349:
2331:
2315:
2286:, is actually a close binary itself. Also in the Cygnus constellation is
2208:
2184:
2028:
1489:
1445:
1360:
1241:
1219:
1062:
984:
905:
712:
696:
530:
310:
167:
117:, or, together with other binaries that change brightness as they orbit,
66:
50:
4714:"Binarity of transit host stars – Implications for planetary parameters"
2818:
1100:
usually (but not always) from the less massive to the more massive star
6680:
5997:
5694:
5667:
5644:
5624:
5609:
5461:
5365:
5343:
5321:
5316:
5180:
4774:
3818:
Kenyon, S. J.; Webbink, R. F. (1984). "The nature of symbiotic stars".
3668:
3233:
2370:
2295:
2287:
2138:
2086:
1855:
1743:
1537:
1449:
1410:
1356:
1307:
While it is not impossible that some binaries might be created through
1118:
1066:
1043:
937:
901:
808:
727:. By 2006, they had been used to give direct distance estimates to the
490: in this section. Unsourced material may be challenged and removed.
391:
363:
187:
183:
144:
140:
98:
4184:
2896:
2745:
948:
that surrounds both stars. As the friction of the envelope brakes the
664:. In the case where the binary is also a spectroscopic binary and the
6184:
6032:
5816:
5781:
5776:
5771:
5731:
5684:
5674:
5468:
5444:
5419:
5326:
5277:
5210:
5200:
5175:
5148:
5124:
5059:
4658:
4425:
Duchêne, Gaspard; Kraus, Adam (August 2013), "Stellar Multiplicity",
4209:
2970:
2477:
2424:
2373:, which is a semidetached binary star system in the constellation of
2345:
2248:
2239:
2212:
2200:
2032:
1481:
1466:
1329:
1209:
581:
387:
339:
171:
82:
4491:
2862:
2671:. New York and London: McGraw-Hill Book Company, Inc. pp. 4–9.
2233:
of binary or ternary stars as a setting, for example, George Lucas'
1476:
In extreme cases this event can cause the white dwarf to exceed the
1184:
The secondary star in a binary star system may be designated as the
465:
135:
to stages that single stars cannot attain. Examples of binaries are
6177:
5878:
5552:
5311:
5284:
4903:
4831:
4319:
4228:
3884:
3839:
3784:
References and discoverer codes, The Washington Double Star Catalog
3632:
3607:
3156:
3131:
2552:
2381:
2234:
2196:
2117:
2101:
1430:
1402:
1359:, meaning that some of its matter ventures into a region where the
1298:
Artist's impression of the evolution of a hot high-mass binary star
665:
449:
338:
Edge-on disc of gas and dust present around the binary star system
230:
219:
6508:
4927:
4735:
4673:
4620:
4439:
4067:"The Formation of Common-Envelope, Pre-Main-Sequence Binary Stars"
3980:
3924:
3647:
Hall, Douglas S. (1989). "The relation between RS CVn and Algol".
3542:
3404:
3248:
6452:
5927:
5689:
5456:
5409:
5392:
5387:
5306:
4605:
4268:
2400:
2276:
2269:
2134:
1812:
1524:
1485:
1257:
1237:
1199:
661:
605:
580:. Most of these cannot be resolved as a visual binary, even with
433:
106:
74:
4356:
Icko, I. (1986). "Binary Star Evolution and Type I Supernovae".
3386:"Galactic distribution of merging neutron stars and black holes"
2163:
While a number of binary star systems have been found to harbor
2100:
Artist's impression of the planets orbiting the primary star of
792:
only be performed on nearby stars, such as those within 10
6556:
6442:
6430:
5649:
5535:
4952:
2395:
stars, 61 Cygni A and 61 Cygni B, which is known for its large
2307:
2230:
2188:
793:
597:
136:
42:
4711:
1409:: when the more massive star became a subgiant, it filled its
747:
Non-eclipsing binaries that can be detected through photometry
4975:
OGLE Atlas of Variable Star Light Curves - Eclipsing binaries
4375:. Lecture Notes in Physics. Vol. 589. pp. 101–122.
3608:"A mechanism for orbital period modulation in close binaries"
2468:
2448:
2291:
1384:
1192:, depending on its temperature relative to the primary star.
831:
precision. Space telescopes can avoid the blurring effect of
669:
541:
Sometimes, the only evidence of a binary star comes from the
526:
522:
412:
234:
203:
179:
175:
78:
4287:
1405:
at a later evolutionary stage. The paradox can be solved by
6539:
5791:
5010:
3817:
3585:
2374:
1688:
1536:
from the center of the first star to the center of mass or
1470:
1229:
1124:
The components of binary stars are denoted by the suffixes
963:
777:
432:
with the primary star at the origin, and the most probable
207:
152:
70:
6492:
4813:"An Ultra Metal-poor Star Near the Hydrogen-burning Limit"
3511:
A Systematic Search of New X-ray Pulsators in ROSAT Fields
2264:
2171:
have shown that most single stars of the same type as the
676:, contains the best-known example of an eclipsing binary.
210:, was discovered to be double by Father Fontenay in 1685.
6157:
2867:
Philosophical Transactions of the Royal Society of London
2726:
Philosophical Transactions of the Royal Society of London
2172:
1806:
1791:
1778:
1767:
1755:
4979:
4212:"Mass Transfer and Disc Formation in AGB Binary Systems"
4061:
2141:, and approximate shape) of both members of the system.
1465:
can occur in a stable manner on the surface through the
4810:
4185:
Vanbeveren, D.; W. van Rensbergen; C. de Loore (2001).
2439:
Planet lost in the glare of binary stars (illustration)
1496:
recently took a picture of the remnants of this event.
1003:, causing the gas to become hotter and emit radiation.
49:
photograph from 2005, with Sirius A in the center, and
147:). Binary stars are also common as the nuclei of many
6719:
4489:
2492:
There are also examples of systems beyond ternaries:
1548:
1505:
of its stars can be determined, for example with the
529:. This animation was assembled from 55 images of the
4578:
American Astronomical Society Meeting Abstracts #229
4273:. American Museum of Natural History. Archived from
3444:
3108:. Stephen F. Austin State University. Archived from
3089:. Stephen F. Austin State University. Archived from
2921:. Dordrecht: D. Reidel Publishing Company. pp.
2027:
It is estimated that approximately one third of the
1671:
is the distance between the two stellar centers, and
1260:
is a 13,000 K white dwarf companion of KOI-81 (
900:
are binary stars where each component is within its
576:, the binaries detected in this manner are known as
362:, by changes in brightness caused by an eclipse; or
252:, a database of visual double stars compiled by the
4928:
IAU Commission G1: Binary and Multiple Star Systems
3696:. Dordrecht: D. Reidel Publishing Company. p.
3173:
Proceedings of the International Astronomical Union
3170:
3004:. D. Reidel Publishing Company, Dordrecht. p.
2698:. Dordrecht: D. Reidel Publishing Company. p.
1031:, high-mass donor star which transfers mass by its
4269:Blondin, J. M.; M. T. Richards; M. L. Malinowski.
1654:
1160:, whose components are ζ Reticuli and ζ Reticuli.
800:, so astrometric binaries will appear to follow a
452:, and hence the distance, of the system is known.
448:can only be expressed in angular units unless the
4216:Monthly Notices of the Royal Astronomical Society
4024:"Planet-hunting telescope unearths hot mysteries"
3391:Monthly Notices of the Royal Astronomical Society
3297:
2524:, "double star", about 240 light-years from Earth
2427:, and containing one of the oldest known stars).
2334:, the first to be discovered. In 2005, using the
2089:, and redder if the brighter star belongs to the
1320:supports the theory that binaries develop during
6779:
1811:(e) Two bodies with similar mass orbiting in an
1703:of the orbit of one body around the other, then
4939:Pictures and news of binaries at Hubblesite.org
4492:"Binary Star Formation from Ring Fragmentation"
3961:
3959:
615:It is impossible to determine individually the
4480:, Harvard-Smithsonian Center for Astrophysics.
4420:
4418:
3599:
2819:Sixth Catalog of Orbits of Visual Binary Stars
2348:, the third closest star system, contains two
2268:The two visibly distinguishable components of
1525:Calculating the center of mass in binary stars
1448:has a close companion star that overflows its
1342:
1117:Artist's impression of the binary star system
838:
6524:
4995:
4017:
4015:
2630:
2555:, a spectroscopic binary with a 3rd component
2314:of −1.46. It is located in the constellation
1172:. These discoverer codes can be found in the
4804:
4601:
4599:
4424:
4069:. Louisiana State University. Archived from
3956:
3369:. San Diego State University. Archived from
3129:
3042:
2646:, Leos Ondra, accessed on line May 26, 2007.
2443:Systems with more than two stars are termed
1737:
1069:), but also hundreds of thousands of years (
796:. Nearby stars often have a relatively high
436:is drawn through these points such that the
402:The brighter star of a visual binary is the
4427:Annual Review of Astronomy and Astrophysics
4415:
4343:Encyclopaedia of Astronomy and Astrophysics
4041:. Dordrecht: Kluwer Academic. p. 355.
3742:, Bob Argyle, ed., London: Springer, 2004,
3164:
2910:
2908:
2906:
2840:
2838:
440:is satisfied. This ellipse is known as the
6531:
6517:
5002:
4988:
4021:
4012:
3759:Entry 14396-6050, discoverer code RHD 1AB,
3383:
3123:
2828:, William I. Hartkopf and Brian D. Mason,
2777:(1997), ed. Kam-Ching Leung, pp. 291–294,
2459:. The name Algol means "demon star" (from
2322:deduced that Sirius was a binary. In 1862
2077:In pairs where the two stars are of equal
2050:There is a direct correlation between the
1163:
823:This method of detecting binaries is also
751:Nearby non-eclipsing binaries can also be
4885:
4848:
4830:
4734:
4705:
4672:
4657:More circumbinary planets are listed in:
4619:
4596:
4507:
4438:
4380:
4301:
4245:
4227:
3979:
3923:
3866:
3640:
3631:
3605:
3541:
3465:
3421:
3403:
3311:
3247:
3202:
3184:
3155:
2944:
2942:
2886:
2594:
2592:
2590:
2430:
2403:(the brightest star in the constellation
553:, with the period of their common orbit.
506:Learn how and when to remove this message
455:
345:
131:can exchange mass, which may bring their
4785:
4642:
4340:
4271:"Mass Transfer in the Binary Star Algol"
3683:
3080:
3078:
3076:
3036:
2903:
2860:
2835:
2722:
2434:
2340:
2263:
2154:
2095:
1420:
1280:
1112:
967:
964:Cataclysmic variables and X-ray binaries
835:, resulting in more precise resolution.
678:
608:, the shape of the curve depends on the
517:
333:
299:
36:
4490:Hubber, D. A.; A. P. Whitworth (2005).
4136:" by Jeff Bryant with Waylena McCully,
3904:
3902:
3513:(Ph.D. thesis). Trieste. Archived from
2956:
2581:
2364:. The visible component belongs to the
2302:, with the optical counterpart being a
1080:
999:onto the compact object. This releases
767:
622:and the inclination of the orbit plane
406:star, and the dimmer is considered the
27:System of two stars orbiting each other
14:
6780:
4370:
3689:
3504:
3445:Smith, Robert Connon (November 2006).
2997:
2962:
2939:
2914:
2794:"Introduction and Growth of the WDS",
2691:
2685:
2664:
2587:
2575:Two-body problem in general relativity
2570:Rotational Brownian motion (astronomy)
1804:
1529:In a simple binary case, the distance
1401:, while the less massive Algol B is a
1132:appended to the system's designation,
995:, gas from the other (donor) star can
268:was first used in this context by Sir
53:, Sirius B, to the left bottom from it
6512:
4983:
4645:"Planets with Two Suns Likely Common"
4546:
4149:
4090:
4039:The Realm of Interacting Binary Stars
3527:
3073:
2658:
2356:An example of an eclipsing binary is
1416:
1011:, the compact object can be either a
651:
4355:
4134:Mass Transfer in Binary Star Systems
4036:
3899:
3740:Observing and Measuring Double Stars
3646:
3065:. Cornell University. Archived from
1821:
537:, sorted according to orbital phase.
488:adding citations to reliable sources
459:
6538:
4935:for amateurs, with orbital elements
4457:10.1146/annurev-astro-081710-102602
4022:Borenstein, Seth (4 January 2010).
3797:. Accessed on line August 20, 2008.
3774:. Accessed on line August 20, 2008.
2832:, accessed on line August 20, 2008.
2809:, accessed on line August 20, 2008.
2548:Habitability of binary star systems
2476:, in the southern constellation of
2464:
2380:Other interesting binaries include
2151:Habitability of binary star systems
1019:. These binaries are classified as
281:By the modern definition, the term
113:each other; these pairs are called
24:
6592:List of most massive star clusters
4788:"Hubble finds mass of white dwarf"
4373:Relativistic Flows in Astrophysics
3761:The Washington Double Star Catalog
3722:"Binary and Multiple Star Systems"
3505:Israel, Gian Luca (October 1996).
3364:
3084:
3060:
2796:The Washington Double Star Catalog
1355:, it may at some point exceed its
369:
329:
151:, and are the progenitors of both
25:
6804:
4921:
3912:The Astrophysical Journal Letters
3103:
1517:in the system. Because this is a
1383:Studies of the eclipsing ternary
1053:
194:in 1650 (and probably earlier by
6765:
6753:
6741:
6729:
6704:
6703:
6491:
6481:
6480:
4970:AAVSO Eclipsing Binaries section
4933:List of the best visual binaries
3423:10.1046/j.1365-8711.2003.06616.x
3278:
3032:. Astronomy. Cornell University.
1805:
1790:
1777:
1766:
1754:
1452:, the white dwarf will steadily
1065:), or a few days (components of
1048:Tolman–Oppenheimer–Volkoff limit
979:When a binary system contains a
875:
861:
847:
464:
223:binary stars and star clusters.
190:), was observed to be double by
85:, in which case they are called
4865:
4779:
4767:
4651:
4636:
4569:
4555:
4540:
4483:
4478:Most Milky Way Stars Are Single
4471:
4364:
4349:
4334:
4281:
4262:
4203:
4178:
4143:
4126:
4109:
4084:
4055:
4030:
3846:
3811:
3800:
3795:United States Naval Observatory
3777:
3772:United States Naval Observatory
3753:
3732:
3714:
3574:
3521:
3498:
3438:
3384:Voss, R.; Tauris, T.M. (2003).
3377:
3358:
3344:
3291:
3281:"Binary neutron star collision"
3272:
3227:
3130:Wilson, R.E. (1 January 2008).
3097:
3054:
3022:
2991:
2854:
2851:, New York: Dover, 1964, p. ix.
2830:United States Naval Observatory
2812:
2807:United States Naval Observatory
2384:(a binary in the constellation
2330:determined that Sirius B was a
1499:
1179:
1103:
475:needs additional citations for
254:United States Naval Observatory
143:(Cygnus X-1 being a well-known
4341:Prialnik, D. (2001). "Novae".
4138:Wolfram Demonstrations Project
4121:Wolfram Demonstrations Project
3530:Astrophysics and Space Science
3050:. New York: Dover. p. 41.
2788:
2760:
2716:
2649:
2608:
2605:, New York: Dover, 1964, p. 1.
2566:, a type of binary star system
1174:Washington Double Star Catalog
1061:can be less than an hour (for
1001:gravitational potential energy
672:, a triple star system in the
250:Washington Double Star Catalog
13:
1:
6597:List of largest star clusters
6393:Timeline of stellar astronomy
4117:Contact Binary Star Envelopes
3612:Astrophysical Journal, Part 1
3507:"Neutron Star X-ray binaries"
2665:Aitken, Robert Grant (1935).
1351:increases in size during its
4691:10.1088/0004-6256/140/6/1657
4496:Astronomy & Astrophysics
4172:10.1016/0083-6656(84)90007-2
3942:10.1088/2041-8205/713/2/L150
3606:Applegate, James H. (1992).
3258:10.1051/epjconf/201510106063
2973:Publishing Company. p.
2081:, they are also of the same
1827:Multiplicity likelihood for
1750:
1302:
1276:
940:. The uppermost part of the
259:
202:). The bright southern star
162:
7:
6604:Hypercompact stellar system
6572:Hypercompact stellar system
6053:Hertzsprung–Russell diagram
4786:McGourty, C. (2005-12-14).
4753:10.1051/0004-6361/200810988
4643:Schirber, M (17 May 2005).
4065:; J. E. Cazes; H. S. Cohl.
2508:
2259:
1815:around a common barycenter
1343:Mass transfer and accretion
974:cataclysmic variable system
952:, the stars may eventually
839:Configuration of the system
41:The well-known binary star
32:Binary Star (hip hop group)
30:For the hip hop group, see
10:
6809:
5967:Kelvin–Helmholtz mechanism
4722:Astronomy and Astrophysics
4549:"Birth and Death of Stars"
4526:10.1051/0004-6361:20042428
3998:10.1088/0004-637X/715/1/51
3354:. University of Tennessee.
2952:. University of Tennessee.
2861:Herschel, William (1802).
2484:in the night sky, with an
2294:source considered to be a
2243:, and one notable story, "
2148:
2144:
1789:
1776:
1765:
1753:
1741:
1140:the secondary. The suffix
1108:
1084:
1005:Cataclysmic variable stars
904:, i.e. the area where the
373:
192:Giovanni Battista Riccioli
29:
6699:
6663:
6627:
6549:
6476:
6401:
6250:
6148:
6076:
5975:
5832:
5707:
5585:
5494:
5230:
5221:
5100:
5030:
5017:
5009:
4944:Chandra X-ray Observatory
4818:The Astrophysical Journal
3968:The Astrophysical Journal
3855:The Astrophysical Journal
3584:. Imagine the Universe!.
3560:10.1007/s10509-008-9839-y
3484:10.1080/00107510601181175
3213:10.1017/S1743921307003845
3136:The Astrophysical Journal
2486:apparent visual magnitude
2054:of a binary star and the
1738:Center-of-mass animations
1270:B-type main-sequence star
1254:A-type main-sequence star
1136:denoting the primary and
972:Artist's conception of a
916:Semidetached binary stars
782:electromagnetic radiation
354:, by periodic changes in
174:. Early examples include
6346:With multiple exoplanets
4850:10.3847/1538-4357/aadd97
4661:The Astronomical Journal
4498:(Submitted manuscript).
3456:(Submitted manuscript).
3087:"Eclipsing Binary Stars"
2615:Vol. 1, part 1, p. 422,
2328:Mount Wilson Observatory
2041:monotonically increasing
1488:, which was observed by
1328:during the formation of
1268:), a 10,000 K late
1252:), a 9,400 K early
584:of the highest existing
272:in 1802, when he wrote:
5132:Asymptotic giant branch
4745:2009A&A...498..567D
4551:. University of Oregon.
4518:2005A&A...437..113H
4449:2013ARA&A..51..269D
4399:10.1007/3-540-46025-X_6
3552:2008Ap&SS.315..335I
3447:"Cataclysmic Variables"
2417:2MASS J18082002−5104378
2068:log normal distribution
1324:. Fragmentation of the
1164:Discoverer designations
604:curve. If the orbit is
390:, or even high-powered
6468:Tidal disruption event
5957:Circumstellar envelope
5191:Luminous blue variable
4358:Cosmogonical Processes
4187:The Brightest Binaries
3690:Heintz, W. D. (1978).
3352:"Astrometric Binaries"
3300:Publ. Astron. Soc. Jpn
3236:EPJ Web of Conferences
2998:Heintz, W. D. (1978).
2963:Heintz, W. D. (1978).
2915:Heintz, W. D. (1978).
2888:10.1098/rstl.1802.0021
2738:10.1098/rstl.1803.0015
2692:Heintz, W. D. (1978).
2440:
2431:Multiple-star examples
2353:
2336:Hubble Space Telescope
2300:high-mass X-ray binary
2272:
2169:Kepler space telescope
2160:
2122:Keplerian harmonic law
2109:
2060:practically in contact
1656:
1494:Hubble Space Telescope
1433:
1313:conservation of energy
1299:
1217:luminous blue variable
1121:
1041:high-mass X-ray binary
976:
692:
600:, then the curve is a
578:spectroscopic binaries
538:
456:Spectroscopic binaries
438:Keplerian law of areas
346:Methods of observation
342:
308:The more general term
305:
279:
241:computed the orbit of
95:spectroscopic binaries
54:
6709:Category:Star systems
6582:Dark globular cluster
5993:Effective temperature
4874:Astrophysical Journal
4608:Extreme Solar Systems
4563:"Binary Star Motions"
4345:. pp. 1846–1856.
4290:Astrophysical Journal
3820:Astrophysical Journal
3649:Space Science Reviews
3330:10.1093/pasj/56.6.L35
2772:ASP Conference Series
2480:, which contains the
2438:
2360:in the constellation
2344:
2267:
2158:
2099:
1657:
1424:
1309:gravitational capture
1297:
1244:companion of KOI-74 (
1116:
971:
927:around the accretor.
804:path across the sky.
706:effective temperature
690:
674:constellation Perseus
658:eclipsing binary star
521:
337:
303:
293:methods are known as
274:
40:
6463:Planet-hosting stars
6341:With resolved images
6312:Historical brightest
6242:Photometric-standard
6168:Solar radio emission
5962:Eddington luminosity
5742:Triple-alpha process
5680:Thorne–Żytkow object
5055:Young stellar object
4565:. Cornell Astronomy.
4247:10.1093/mnras/stx680
3517:on 10 December 2008.
3454:Contemporary Physics
3119:on 3 September 2003.
2582:Notes and references
2482:third-brightest star
2114:gravitational lenses
2052:period of revolution
1546:
1507:binary mass function
1425:Artist rendering of
1081:Variations in period
774:Astrometric binaries
768:Astrometric binaries
758:relativistic beaming
535:near-infrared H-band
531:CHARA interferometer
484:improve this article
289:with a telescope or
119:photometric binaries
103:astrometric binaries
18:Spectroscopic binary
6640:Stellar association
6287:Highest temperature
6058:Color–color diagram
5923:Protoplanetary disk
5727:Proton–proton chain
5405:Chemically peculiar
4896:2007ApJ...660..807Q
4841:2018ApJ...867...98S
4683:2010AJ....140.1657M
4630:2008ASPC..398..201Q
4590:2017AAS...22921905K
4391:2002LNP...589..101F
4312:2000ApJ...544L.133H
4238:2017MNRAS.468.4465C
4164:1984VA.....27..149B
4152:Vistas in Astronomy
4095:. Kluwer Academic.
3990:2010ApJ...715...51V
3934:2010ApJ...713L.150R
3877:2005ApJ...633L..37I
3832:1984ApJ...279..252K
3661:1989SSRv...50..219H
3624:1992ApJ...385..621A
3476:2007astro.ph..1654S
3414:2003MNRAS.342.1169V
3322:2004PASJ...56L..35A
3195:2007IAUS..240...79B
3148:2008ApJ...672..575W
2879:1802RSPT...92..477H
2849:Robert Grant Aitken
2783:1997ASPC..130..291S
2637:A New View of Mizar
2603:Robert Grant Aitken
2543:Circumbinary planet
2538:Binary brown dwarfs
2457:Geminiano Montanari
2229:has often featured
1835:
1699:is taken to be the
1478:Chandrasekhar limit
1335:The outcome of the
1240:is a 12,000 K
1087:Applegate mechanism
942:stellar atmospheres
6655:Hypervelocity star
6292:Lowest temperature
6043:Photometric system
6013:Absolute magnitude
5947:Circumstellar dust
5560:Stellar black hole
5196:Stellar population
5082:Herbig–Haro object
4963:2007-10-16 at the
4119:" by Jeff Bryant,
4091:Kopal, Z. (1989).
3789:2011-05-17 at the
3669:10.1007/BF00215932
2824:2009-04-12 at the
2801:2008-09-17 at the
2642:2008-03-07 at the
2623:2011-08-10 at the
2441:
2419:(a binary in the "
2388:, composed of two
2354:
2324:Alvan Graham Clark
2312:apparent magnitude
2273:
2165:extrasolar planets
2161:
2110:
2106:triple star system
1826:
1652:
1519:conserved quantity
1434:
1417:Runaways and novae
1361:gravitational pull
1349:main-sequence star
1337:three-body problem
1300:
1122:
1093:main-sequence star
977:
906:gravitational pull
833:Earth's atmosphere
828:extrasolar planets
702:surface brightness
693:
652:Eclipsing binaries
539:
396:angular resolution
343:
306:
196:Benedetto Castelli
157:type Ia supernovae
115:eclipsing binaries
63:binary star system
55:
6717:
6716:
6506:
6505:
6409:Substellar object
6388:Planetary nebulae
5807:Luminous red nova
5717:Deuterium burning
5703:
5702:
5186:Instability strip
5166:Wolf-Rayet nebula
5120:Horizontal branch
5065:Pre-main-sequence
4408:978-3-540-43518-1
4196:978-0-7923-5155-9
4102:978-0-7923-0129-5
4093:The Roche Problem
4048:978-0-7923-1675-6
3707:978-90-277-0885-4
3373:on 23 March 2007.
3287:on 26 April 2012.
3093:on 14 April 2007.
3015:978-90-277-0885-4
2984:978-90-277-0885-4
2950:"Visual Binaries"
2932:978-90-277-0885-4
2709:978-90-277-0885-4
2533:Binary black hole
2518:, possible binary
2025:
2024:
1822:Research findings
1819:
1818:
1785:Earth–Moon system
1691:of the two stars.
1647:
1644:
1605:
1459:degenerate matter
1395:stellar evolution
1393:in the theory of
1295:
1154:Bayer designation
898:Detached binaries
741:Triangulum Galaxy
688:
631: sin
568:by observing the
516:
515:
508:
430:polar coordinates
352:spectroscopically
149:planetary nebulae
45:, seen here in a
16:(Redirected from
6800:
6770:
6769:
6768:
6758:
6757:
6756:
6746:
6745:
6744:
6734:
6733:
6732:
6725:
6707:
6706:
6619:Planetary system
6577:Globular cluster
6533:
6526:
6519:
6510:
6509:
6498:Stars portal
6496:
6495:
6484:
6483:
6140:Planetary system
6063:Strömgren sphere
5935:Asteroseismology
5656:Black hole star
5228:
5227:
5154:Planetary nebula
5115:Red-giant branch
5004:
4997:
4990:
4981:
4980:
4916:
4915:
4889:
4887:astro-ph/0701266
4869:
4863:
4862:
4852:
4834:
4808:
4802:
4801:
4799:
4798:
4783:
4777:
4771:
4765:
4764:
4738:
4718:
4709:
4703:
4702:
4676:
4655:
4649:
4648:
4640:
4634:
4633:
4623:
4603:
4594:
4593:
4573:
4567:
4566:
4559:
4553:
4552:
4544:
4538:
4537:
4511:
4509:astro-ph/0503412
4487:
4481:
4475:
4469:
4467:
4442:
4422:
4413:
4412:
4384:
4382:astro-ph/0109502
4368:
4362:
4361:
4353:
4347:
4346:
4338:
4332:
4331:
4305:
4303:astro-ph/0007436
4285:
4279:
4278:
4266:
4260:
4259:
4249:
4231:
4222:(4): 4465–4477.
4207:
4201:
4200:
4182:
4176:
4175:
4147:
4141:
4130:
4124:
4113:
4107:
4106:
4088:
4082:
4081:
4079:
4078:
4059:
4053:
4052:
4034:
4028:
4027:
4019:
4010:
4009:
3983:
3963:
3954:
3953:
3927:
3918:(2): L150–L154.
3906:
3897:
3896:
3870:
3868:astro-ph/0510581
3850:
3844:
3843:
3815:
3809:
3804:
3798:
3781:
3775:
3757:
3751:
3736:
3730:
3729:
3718:
3712:
3711:
3687:
3681:
3680:
3655:(1–2): 219–233.
3644:
3638:
3637:
3635:
3603:
3597:
3596:
3594:
3592:
3578:
3572:
3571:
3545:
3536:(1–4): 335–340.
3525:
3519:
3518:
3502:
3496:
3495:
3469:
3467:astro-ph/0701654
3451:
3442:
3436:
3435:
3425:
3407:
3398:(4): 1169–1184.
3381:
3375:
3374:
3362:
3356:
3355:
3348:
3342:
3341:
3315:
3313:astro-ph/0409613
3295:
3289:
3288:
3276:
3270:
3269:
3251:
3231:
3225:
3224:
3206:
3188:
3186:astro-ph/0610923
3168:
3162:
3161:
3159:
3127:
3121:
3120:
3118:
3101:
3095:
3094:
3082:
3071:
3070:
3069:on 17 June 2012.
3063:"Stellar Masses"
3058:
3052:
3051:
3048:The Binary Stars
3040:
3034:
3033:
3026:
3020:
3019:
2995:
2989:
2988:
2960:
2954:
2953:
2946:
2937:
2936:
2912:
2901:
2900:
2890:
2858:
2852:
2845:The Binary Stars
2842:
2833:
2816:
2810:
2792:
2786:
2764:
2758:
2757:
2720:
2714:
2713:
2689:
2683:
2682:
2668:The Binary Stars
2662:
2656:
2653:
2647:
2634:
2628:
2617:Almagestum Novum
2612:
2606:
2599:The Binary Stars
2596:
2466:
2390:K class (orange)
2320:Friedrich Bessel
2219:, among others.
2118:stellar parallax
2021:
2019:
1998:
1996:
1986:
1973:
1971:
1961:
1948:
1946:
1939:
1937:
1930:
1917:
1915:
1908:
1906:
1899:
1886:
1885:
1884:
1874:
1873:
1872:
1836:
1825:
1809:
1798:Sun–Earth system
1794:
1781:
1770:
1758:
1751:
1733:
1661:
1659:
1658:
1653:
1648:
1646:
1645:
1643:
1642:
1633:
1632:
1623:
1611:
1606:
1604:
1603:
1602:
1590:
1589:
1579:
1578:
1569:
1558:
1557:
1515:angular momentum
1427:plasma ejections
1370:Lagrangian point
1296:
1071:Proxima Centauri
879:
865:
851:
784:, for example a
737:Andromeda Galaxy
725:standard candles
717:orbital elements
689:
635:
511:
504:
500:
497:
491:
468:
460:
450:stellar parallax
442:apparent ellipse
270:William Herschel
243:Xi Ursae Majoris
227:William Herschel
182:. Mizar, in the
77:bound to and in
21:
6808:
6807:
6803:
6802:
6801:
6799:
6798:
6797:
6778:
6777:
6776:
6766:
6764:
6754:
6752:
6742:
6740:
6730:
6728:
6720:
6718:
6713:
6695:
6664:Visual grouping
6659:
6623:
6545:
6537:
6507:
6502:
6490:
6472:
6397:
6366:Milky Way novae
6302:Smallest volume
6246:
6227:Radial velocity
6150:
6144:
6096:Common envelope
6072:
5971:
5940:Helioseismology
5911:Bipolar outflow
5852:Microturbulence
5847:Convection zone
5828:
5722:Lithium burning
5709:Nucleosynthesis
5699:
5581:
5490:
5217:
5096:
5045:Molecular cloud
5026:
5013:
5008:
4965:Wayback Machine
4924:
4919:
4870:
4866:
4809:
4805:
4796:
4794:
4784:
4780:
4773:See sources at
4772:
4768:
4716:
4710:
4706:
4656:
4652:
4641:
4637:
4604:
4597:
4574:
4570:
4561:
4560:
4556:
4545:
4541:
4488:
4484:
4476:
4472:
4423:
4416:
4409:
4369:
4365:
4354:
4350:
4339:
4335:
4286:
4282:
4267:
4263:
4208:
4204:
4197:
4183:
4179:
4148:
4144:
4131:
4127:
4114:
4110:
4103:
4089:
4085:
4076:
4074:
4060:
4056:
4049:
4035:
4031:
4020:
4013:
3964:
3957:
3907:
3900:
3851:
3847:
3816:
3812:
3805:
3801:
3791:Wayback Machine
3782:
3778:
3758:
3754:
3737:
3733:
3720:
3719:
3715:
3708:
3688:
3684:
3645:
3641:
3604:
3600:
3590:
3588:
3580:
3579:
3575:
3526:
3522:
3503:
3499:
3449:
3443:
3439:
3382:
3378:
3363:
3359:
3350:
3349:
3345:
3296:
3292:
3277:
3273:
3232:
3228:
3204:10.1.1.254.2692
3169:
3165:
3128:
3124:
3112:
3102:
3098:
3083:
3074:
3059:
3055:
3041:
3037:
3028:
3027:
3023:
3016:
2996:
2992:
2985:
2961:
2957:
2948:
2947:
2940:
2933:
2913:
2904:
2859:
2855:
2843:
2836:
2826:Wayback Machine
2817:
2813:
2803:Wayback Machine
2793:
2789:
2765:
2761:
2721:
2717:
2710:
2690:
2686:
2679:
2663:
2659:
2654:
2650:
2644:Wayback Machine
2635:
2631:
2625:Wayback Machine
2613:
2609:
2597:
2588:
2584:
2579:
2559:Hills mechanism
2511:
2433:
2358:Epsilon Aurigae
2262:
2227:Science fiction
2153:
2147:
2017:
2015:
2009:
2006:
1994:
1992:
1985:
1982:
1978:
1969:
1967:
1960:
1957:
1953:
1944:
1942:
1935:
1933:
1929:
1926:
1922:
1913:
1911:
1904:
1902:
1898:
1895:
1891:
1882:
1880:
1879:
1877:
1870:
1868:
1867:
1865:
1861:
1858:
1848:
1843:
1824:
1810:
1795:
1782:
1771:
1759:
1746:
1740:
1732:
1721:
1715:
1709:
1686:
1679:
1638:
1634:
1628:
1624:
1622:
1615:
1610:
1598:
1594:
1585:
1581:
1580:
1574:
1570:
1568:
1553:
1549:
1547:
1544:
1543:
1535:
1527:
1502:
1463:Hydrogen fusion
1419:
1345:
1326:molecular cloud
1305:
1281:
1279:
1224:Wolf–Rayet star
1206:Symbiotic stars
1182:
1166:
1111:
1106:
1089:
1083:
1059:Orbital periods
1056:
966:
960:is an example.
958:W Ursae Majoris
946:common envelope
892:
891:
890:
889:
885:
884:
883:
880:
871:
870:
869:
866:
857:
856:
855:
852:
841:
770:
756:looking at how
753:photometrically
749:
679:
654:
627:
617:semi-major axis
586:resolving power
562:radial velocity
512:
501:
495:
492:
481:
469:
458:
446:semi-major axis
378:
372:
370:Visual binaries
364:astrometrically
360:photometrically
348:
332:
330:Classifications
320:optical doubles
295:visual binaries
291:interferometric
262:
165:
87:visual binaries
75:gravitationally
35:
28:
23:
22:
15:
12:
11:
5:
6806:
6796:
6795:
6790:
6775:
6774:
6762:
6750:
6738:
6715:
6714:
6712:
6711:
6700:
6697:
6696:
6694:
6693:
6688:
6683:
6678:
6673:
6667:
6665:
6661:
6660:
6658:
6657:
6652:
6647:
6642:
6637:
6635:Stellar stream
6631:
6629:
6625:
6624:
6622:
6621:
6616:
6611:
6606:
6601:
6600:
6599:
6594:
6589:
6584:
6579:
6574:
6564:
6559:
6553:
6551:
6547:
6546:
6536:
6535:
6528:
6521:
6513:
6504:
6503:
6501:
6500:
6488:
6477:
6474:
6473:
6471:
6470:
6465:
6460:
6455:
6450:
6445:
6440:
6435:
6434:
6433:
6428:
6427:
6426:
6421:
6405:
6403:
6399:
6398:
6396:
6395:
6390:
6385:
6384:
6383:
6378:
6368:
6363:
6358:
6353:
6348:
6343:
6338:
6337:
6336:
6331:
6330:
6329:
6319:
6314:
6309:
6304:
6299:
6297:Largest volume
6294:
6289:
6284:
6274:
6273:
6272:
6267:
6256:
6254:
6248:
6247:
6245:
6244:
6239:
6234:
6229:
6224:
6223:
6222:
6217:
6212:
6202:
6197:
6192:
6187:
6182:
6181:
6180:
6175:
6170:
6165:
6154:
6152:
6146:
6145:
6143:
6142:
6137:
6136:
6135:
6130:
6125:
6115:
6110:
6109:
6108:
6103:
6098:
6093:
6082:
6080:
6074:
6073:
6071:
6070:
6065:
6060:
6055:
6050:
6045:
6040:
6035:
6030:
6025:
6020:
6015:
6010:
6008:Magnetic field
6005:
6000:
5995:
5990:
5985:
5979:
5977:
5973:
5972:
5970:
5969:
5964:
5959:
5954:
5949:
5944:
5943:
5942:
5932:
5931:
5930:
5925:
5918:Accretion disk
5915:
5914:
5913:
5908:
5898:
5897:
5896:
5894:Alfvén surface
5891:
5889:Stellar corona
5886:
5881:
5876:
5866:
5864:Radiation zone
5861:
5860:
5859:
5854:
5844:
5838:
5836:
5830:
5829:
5827:
5826:
5821:
5820:
5819:
5814:
5809:
5804:
5799:
5789:
5784:
5779:
5774:
5769:
5764:
5759:
5754:
5749:
5744:
5739:
5734:
5729:
5724:
5719:
5713:
5711:
5705:
5704:
5701:
5700:
5698:
5697:
5692:
5687:
5682:
5677:
5672:
5671:
5670:
5665:
5662:
5654:
5653:
5652:
5647:
5642:
5637:
5632:
5627:
5622:
5617:
5612:
5602:
5597:
5591:
5589:
5583:
5582:
5580:
5579:
5574:
5573:
5572:
5562:
5557:
5556:
5555:
5550:
5549:
5548:
5543:
5533:
5523:
5522:
5521:
5511:
5506:
5500:
5498:
5492:
5491:
5489:
5488:
5486:Blue straggler
5483:
5482:
5481:
5471:
5466:
5465:
5464:
5454:
5453:
5452:
5447:
5442:
5437:
5432:
5427:
5422:
5417:
5412:
5402:
5397:
5396:
5395:
5390:
5385:
5375:
5374:
5373:
5363:
5362:
5361:
5356:
5351:
5341:
5336:
5335:
5334:
5329:
5324:
5314:
5309:
5304:
5299:
5298:
5297:
5292:
5282:
5281:
5280:
5275:
5270:
5265:
5260:
5255:
5250:
5244:Main sequence
5242:
5237:
5231:
5225:
5223:Classification
5219:
5218:
5216:
5215:
5214:
5213:
5208:
5198:
5193:
5188:
5183:
5178:
5173:
5168:
5163:
5162:
5161:
5159:Protoplanetary
5151:
5146:
5145:
5144:
5139:
5129:
5128:
5127:
5117:
5112:
5106:
5104:
5098:
5097:
5095:
5094:
5089:
5084:
5079:
5078:
5077:
5072:
5067:
5062:
5052:
5047:
5042:
5036:
5034:
5028:
5027:
5025:
5024:
5018:
5015:
5014:
5007:
5006:
4999:
4992:
4984:
4978:
4977:
4972:
4967:
4955:
4946:
4941:
4936:
4930:
4923:
4922:External links
4920:
4918:
4917:
4904:10.1086/512542
4880:(1): 807–822.
4864:
4803:
4778:
4766:
4729:(2): 567–574.
4704:
4650:
4635:
4595:
4568:
4554:
4547:Schombert, J.
4539:
4502:(1): 113–125.
4482:
4470:
4468:. See Table 1.
4433:(1): 269–310,
4414:
4407:
4363:
4360:. p. 155.
4348:
4333:
4320:10.1086/317315
4280:
4277:on 2006-04-08.
4261:
4202:
4195:
4177:
4158:(2): 149–169.
4142:
4125:
4108:
4101:
4083:
4063:Tohline, J. E.
4054:
4047:
4029:
4026:(6:29 pm EST).
4011:
3955:
3898:
3885:10.1086/498268
3861:(1): L37–L40.
3845:
3840:10.1086/161888
3810:
3799:
3776:
3766:2012-07-08 at
3752:
3731:
3728:on 2006-02-07.
3713:
3706:
3682:
3639:
3633:10.1086/170967
3598:
3573:
3520:
3497:
3460:(6): 363–386.
3437:
3376:
3357:
3343:
3306:(6): L35–L38.
3290:
3271:
3226:
3163:
3157:10.1086/523634
3142:(1): 575–589.
3122:
3106:"Binary Stars"
3096:
3072:
3053:
3035:
3030:"Binary Stars"
3021:
3014:
2990:
2983:
2955:
2938:
2931:
2902:
2853:
2834:
2811:
2787:
2759:
2715:
2708:
2684:
2678:978-1117504094
2677:
2657:
2648:
2629:
2607:
2585:
2583:
2580:
2578:
2577:
2572:
2567:
2564:Heartbeat star
2561:
2556:
2550:
2545:
2540:
2535:
2530:
2525:
2519:
2512:
2510:
2507:
2474:Alpha Centauri
2445:multiple stars
2432:
2429:
2366:spectral class
2261:
2258:
2149:Main article:
2146:
2143:
2072:star formation
2037:ordinary stars
2023:
2022:
2013:
2010:
2007:
2004:
2000:
1999:
1990:
1987:
1983:
1980:
1975:
1974:
1965:
1962:
1958:
1955:
1950:
1949:
1940:
1931:
1927:
1924:
1919:
1918:
1909:
1900:
1896:
1893:
1888:
1887:
1875:
1863:
1859:
1856:
1851:
1850:
1845:
1840:
1823:
1820:
1817:
1816:
1802:
1801:
1788:
1774:
1773:
1764:
1742:Main article:
1739:
1736:
1730:
1719:
1707:
1701:semimajor axis
1693:
1692:
1684:
1677:
1672:
1651:
1641:
1637:
1631:
1627:
1621:
1618:
1614:
1609:
1601:
1597:
1593:
1588:
1584:
1577:
1573:
1567:
1564:
1561:
1556:
1552:
1533:
1526:
1523:
1501:
1498:
1480:and trigger a
1418:
1415:
1366:accretion disc
1344:
1341:
1322:star formation
1304:
1301:
1278:
1275:
1274:
1273:
1234:Kepler mission
1227:
1213:
1203:
1190:cool companion
1181:
1178:
1165:
1162:
1110:
1107:
1105:
1102:
1085:Main article:
1082:
1079:
1075:Alpha Centauri
1055:
1054:Orbital period
1052:
1009:X-ray binaries
981:compact object
965:
962:
950:orbital motion
933:contact binary
925:accretion disc
887:
886:
881:
874:
873:
872:
867:
860:
859:
858:
853:
846:
845:
844:
843:
842:
840:
837:
825:used to locate
769:
766:
748:
745:
653:
650:
574:spectral lines
572:of the stars'
551:center of mass
547:spectral lines
543:Doppler effect
514:
513:
472:
470:
463:
457:
454:
425:position angle
374:Main article:
371:
368:
356:spectral lines
347:
344:
340:HD 106906
331:
328:
316:binary systems
261:
258:
208:Southern Cross
164:
161:
128:binary systems
26:
9:
6:
4:
3:
2:
6805:
6794:
6791:
6789:
6786:
6785:
6783:
6773:
6763:
6761:
6751:
6749:
6739:
6737:
6727:
6726:
6723:
6710:
6702:
6701:
6698:
6692:
6691:Constellation
6689:
6687:
6684:
6682:
6679:
6677:
6676:Multiple star
6674:
6672:
6669:
6668:
6666:
6662:
6656:
6653:
6651:
6648:
6646:
6643:
6641:
6638:
6636:
6633:
6632:
6630:
6626:
6620:
6617:
6615:
6612:
6610:
6607:
6605:
6602:
6598:
6595:
6593:
6590:
6588:
6585:
6583:
6580:
6578:
6575:
6573:
6570:
6569:
6568:
6565:
6563:
6560:
6558:
6555:
6554:
6552:
6548:
6544:
6541:
6534:
6529:
6527:
6522:
6520:
6515:
6514:
6511:
6499:
6494:
6489:
6487:
6479:
6478:
6475:
6469:
6466:
6464:
6461:
6459:
6458:Intergalactic
6456:
6454:
6451:
6449:
6446:
6444:
6441:
6439:
6438:Galactic year
6436:
6432:
6429:
6425:
6422:
6420:
6417:
6416:
6415:
6412:
6411:
6410:
6407:
6406:
6404:
6400:
6394:
6391:
6389:
6386:
6382:
6379:
6377:
6374:
6373:
6372:
6369:
6367:
6364:
6362:
6359:
6357:
6354:
6352:
6349:
6347:
6344:
6342:
6339:
6335:
6332:
6328:
6325:
6324:
6323:
6320:
6318:
6317:Most luminous
6315:
6313:
6310:
6308:
6305:
6303:
6300:
6298:
6295:
6293:
6290:
6288:
6285:
6283:
6280:
6279:
6278:
6275:
6271:
6268:
6266:
6263:
6262:
6261:
6258:
6257:
6255:
6253:
6249:
6243:
6240:
6238:
6235:
6233:
6232:Proper motion
6230:
6228:
6225:
6221:
6218:
6216:
6213:
6211:
6208:
6207:
6206:
6203:
6201:
6198:
6196:
6195:Constellation
6193:
6191:
6188:
6186:
6183:
6179:
6176:
6174:
6171:
6169:
6166:
6164:
6163:Solar eclipse
6161:
6160:
6159:
6156:
6155:
6153:
6149:Earth-centric
6147:
6141:
6138:
6134:
6131:
6129:
6126:
6124:
6121:
6120:
6119:
6116:
6114:
6111:
6107:
6104:
6102:
6099:
6097:
6094:
6092:
6089:
6088:
6087:
6084:
6083:
6081:
6079:
6075:
6069:
6066:
6064:
6061:
6059:
6056:
6054:
6051:
6049:
6046:
6044:
6041:
6039:
6036:
6034:
6031:
6029:
6026:
6024:
6021:
6019:
6016:
6014:
6011:
6009:
6006:
6004:
6001:
5999:
5996:
5994:
5991:
5989:
5986:
5984:
5981:
5980:
5978:
5974:
5968:
5965:
5963:
5960:
5958:
5955:
5953:
5950:
5948:
5945:
5941:
5938:
5937:
5936:
5933:
5929:
5926:
5924:
5921:
5920:
5919:
5916:
5912:
5909:
5907:
5904:
5903:
5902:
5899:
5895:
5892:
5890:
5887:
5885:
5882:
5880:
5877:
5875:
5872:
5871:
5870:
5867:
5865:
5862:
5858:
5855:
5853:
5850:
5849:
5848:
5845:
5843:
5840:
5839:
5837:
5835:
5831:
5825:
5822:
5818:
5815:
5813:
5810:
5808:
5805:
5803:
5800:
5798:
5795:
5794:
5793:
5790:
5788:
5785:
5783:
5780:
5778:
5775:
5773:
5770:
5768:
5765:
5763:
5760:
5758:
5755:
5753:
5750:
5748:
5747:Alpha process
5745:
5743:
5740:
5738:
5735:
5733:
5730:
5728:
5725:
5723:
5720:
5718:
5715:
5714:
5712:
5710:
5706:
5696:
5693:
5691:
5688:
5686:
5683:
5681:
5678:
5676:
5673:
5669:
5666:
5663:
5661:
5658:
5657:
5655:
5651:
5648:
5646:
5643:
5641:
5638:
5636:
5633:
5631:
5628:
5626:
5623:
5621:
5618:
5616:
5613:
5611:
5608:
5607:
5606:
5603:
5601:
5598:
5596:
5593:
5592:
5590:
5588:
5584:
5578:
5575:
5571:
5568:
5567:
5566:
5563:
5561:
5558:
5554:
5551:
5547:
5544:
5542:
5539:
5538:
5537:
5534:
5532:
5529:
5528:
5527:
5524:
5520:
5519:Helium planet
5517:
5516:
5515:
5512:
5510:
5509:Parker's star
5507:
5505:
5502:
5501:
5499:
5497:
5493:
5487:
5484:
5480:
5477:
5476:
5475:
5472:
5470:
5467:
5463:
5460:
5459:
5458:
5455:
5451:
5448:
5446:
5443:
5441:
5440:Lambda Boötis
5438:
5436:
5433:
5431:
5428:
5426:
5423:
5421:
5418:
5416:
5413:
5411:
5408:
5407:
5406:
5403:
5401:
5398:
5394:
5391:
5389:
5386:
5384:
5381:
5380:
5379:
5376:
5372:
5369:
5368:
5367:
5364:
5360:
5357:
5355:
5352:
5350:
5347:
5346:
5345:
5342:
5340:
5337:
5333:
5330:
5328:
5325:
5323:
5320:
5319:
5318:
5315:
5313:
5310:
5308:
5305:
5303:
5300:
5296:
5293:
5291:
5288:
5287:
5286:
5283:
5279:
5276:
5274:
5271:
5269:
5266:
5264:
5261:
5259:
5256:
5254:
5251:
5249:
5246:
5245:
5243:
5241:
5238:
5236:
5233:
5232:
5229:
5226:
5224:
5220:
5212:
5209:
5207:
5206:Superluminous
5204:
5203:
5202:
5199:
5197:
5194:
5192:
5189:
5187:
5184:
5182:
5179:
5177:
5174:
5172:
5169:
5167:
5164:
5160:
5157:
5156:
5155:
5152:
5150:
5147:
5143:
5140:
5138:
5135:
5134:
5133:
5130:
5126:
5123:
5122:
5121:
5118:
5116:
5113:
5111:
5110:Main sequence
5108:
5107:
5105:
5103:
5099:
5093:
5090:
5088:
5087:Hayashi track
5085:
5083:
5080:
5076:
5073:
5071:
5068:
5066:
5063:
5061:
5058:
5057:
5056:
5053:
5051:
5048:
5046:
5043:
5041:
5038:
5037:
5035:
5033:
5029:
5023:
5020:
5019:
5016:
5012:
5005:
5000:
4998:
4993:
4991:
4986:
4985:
4982:
4976:
4973:
4971:
4968:
4966:
4962:
4959:
4956:
4954:
4950:
4947:
4945:
4942:
4940:
4937:
4934:
4931:
4929:
4926:
4925:
4913:
4909:
4905:
4901:
4897:
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4073:on 2016-06-04
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3769:
3768:archive.today
3765:
3762:
3756:
3749:
3748:1-85233-558-0
3745:
3741:
3738:pp. 307–308,
3735:
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3587:
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3582:"Black Holes"
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3367:"Roche model"
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2969:. Dordrecht:
2968:
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2531:
2529:
2528:Beta Centauri
2526:
2523:
2520:
2517:
2514:
2513:
2506:
2504:
2499:
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2487:
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2428:
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2402:
2398:
2397:proper motion
2394:
2393:main-sequence
2391:
2387:
2383:
2378:
2376:
2372:
2367:
2363:
2359:
2351:
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2343:
2339:
2337:
2333:
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2321:
2317:
2313:
2309:
2305:
2304:variable star
2301:
2297:
2293:
2289:
2285:
2282:
2281:constellation
2278:
2271:
2266:
2257:
2255:
2250:
2246:
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2236:
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2206:
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2190:
2186:
2181:
2178:
2174:
2170:
2166:
2157:
2152:
2142:
2140:
2136:
2131:
2125:
2123:
2119:
2115:
2107:
2103:
2098:
2094:
2092:
2091:main sequence
2088:
2084:
2083:spectral type
2080:
2075:
2073:
2069:
2065:
2064:proper motion
2061:
2057:
2053:
2048:
2046:
2042:
2038:
2034:
2030:
2014:
2011:
2002:
2001:
1991:
1988:
1977:
1976:
1966:
1963:
1952:
1951:
1941:
1932:
1923:0.7–1.3
1921:
1920:
1910:
1901:
1892:0.1–0.5
1890:
1889:
1876:
1864:
1862:
1853:
1852:
1846:
1841:
1838:
1837:
1833:
1832:main-sequence
1830:
1814:
1808:
1803:
1799:
1793:
1786:
1780:
1775:
1769:
1763:
1757:
1752:
1749:
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1702:
1698:
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1676:
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1522:
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1508:
1497:
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1491:
1487:
1483:
1479:
1474:
1472:
1468:
1464:
1460:
1455:
1451:
1447:
1442:
1440:
1439:runaway stars
1432:
1428:
1423:
1414:
1412:
1408:
1407:mass transfer
1404:
1400:
1399:main sequence
1396:
1392:
1391:
1390:Algol paradox
1386:
1381:
1379:
1373:
1371:
1367:
1362:
1358:
1354:
1350:
1340:
1338:
1333:
1331:
1327:
1323:
1319:
1318:main sequence
1314:
1310:
1271:
1267:
1263:
1259:
1255:
1251:
1247:
1243:
1239:
1235:
1231:
1228:
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1221:
1218:
1214:
1211:
1207:
1204:
1201:
1198:
1197:
1196:
1193:
1191:
1187:
1186:hot companion
1177:
1175:
1171:
1161:
1159:
1158:Zeta Reticuli
1155:
1151:
1147:
1143:
1139:
1135:
1131:
1127:
1120:
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1101:
1097:
1094:
1088:
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1038:
1034:
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1022:
1018:
1014:
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1006:
1002:
998:
994:
990:
986:
982:
975:
970:
961:
959:
955:
951:
947:
943:
939:
935:
934:
928:
926:
922:
921:mass transfer
917:
913:
911:
910:main sequence
907:
903:
899:
895:
878:
864:
850:
836:
834:
829:
826:
821:
819:
815:
810:
805:
803:
799:
798:proper motion
795:
789:
787:
783:
779:
775:
765:
763:
759:
754:
744:
742:
738:
734:
730:
726:
720:
718:
714:
709:
707:
703:
698:
677:
675:
671:
667:
663:
659:
649:
645:
643:
639:
634:
630:
625:
621:
618:
613:
611:
607:
603:
599:
593:
589:
587:
583:
579:
575:
571:
570:Doppler shift
567:
563:
559:
558:perpendicular
554:
552:
548:
544:
536:
532:
528:
524:
520:
510:
507:
499:
489:
485:
479:
478:
473:This section
471:
467:
462:
461:
453:
451:
447:
443:
439:
435:
431:
426:
421:
419:
415:
414:
409:
405:
400:
397:
393:
389:
385:
384:
383:visual binary
377:
376:Visual binary
367:
365:
361:
357:
353:
341:
336:
327:
325:
324:optical pairs
321:
317:
313:
312:
302:
298:
296:
292:
288:
284:
278:
273:
271:
267:
257:
255:
251:
246:
244:
240:
236:
232:
228:
224:
221:
216:
211:
209:
205:
201:
197:
193:
189:
185:
181:
177:
173:
169:
160:
158:
154:
150:
146:
142:
138:
134:
130:
129:
122:
120:
116:
112:
108:
104:
100:
96:
92:
88:
84:
80:
76:
72:
68:
64:
60:
52:
48:
44:
39:
33:
19:
6788:Binary stars
6772:Solar System
6650:Runaway star
6645:Moving group
6613:
6587:Open cluster
6567:Star cluster
6562:Dwarf galaxy
6361:White dwarfs
6351:Brown dwarfs
6334:Most distant
6282:Most massive
6260:Proper names
6220:Photographic
6173:Solar System
6151:observations
6085:
6078:Star systems
5901:Stellar wind
5884:Chromosphere
5857:Oscillations
5737:Helium flash
5587:Hypothetical
5565:X-ray binary
5504:Compact star
5339:Bright giant
5092:Henyey track
5070:Herbig Ae/Be
4949:Binary Stars
4877:
4873:
4867:
4822:
4816:
4806:
4795:. Retrieved
4791:
4781:
4769:
4726:
4720:
4707:
4664:
4660:
4653:
4647:. Space.com.
4638:
4611:
4607:
4581:
4577:
4571:
4557:
4542:
4499:
4495:
4485:
4473:
4430:
4426:
4372:
4366:
4357:
4351:
4342:
4336:
4293:
4289:
4283:
4275:the original
4264:
4219:
4215:
4205:
4189:. Springer.
4186:
4180:
4155:
4151:
4145:
4128:
4111:
4092:
4086:
4075:. Retrieved
4071:the original
4057:
4038:
4032:
3974:(1): 51–58.
3971:
3967:
3915:
3911:
3858:
3854:
3848:
3823:
3819:
3813:
3802:
3779:
3755:
3739:
3734:
3726:the original
3716:
3693:Double Stars
3692:
3685:
3652:
3648:
3642:
3615:
3611:
3601:
3589:. Retrieved
3576:
3533:
3529:
3523:
3515:the original
3510:
3500:
3457:
3453:
3440:
3395:
3389:
3379:
3371:the original
3360:
3346:
3303:
3299:
3293:
3285:the original
3274:
3239:
3235:
3229:
3176:
3172:
3166:
3139:
3135:
3125:
3110:the original
3099:
3091:the original
3067:the original
3056:
3047:
3044:Aitken, R.G.
3038:
3024:
3001:Double Stars
3000:
2993:
2966:Double Stars
2965:
2958:
2918:Double Stars
2917:
2873:: 477–528 .
2870:
2866:
2856:
2844:
2814:
2790:
2774:
2771:
2767:
2762:
2729:
2725:
2718:
2695:Double Stars
2694:
2687:
2667:
2660:
2651:
2632:
2616:
2610:
2598:
2491:
2467:
2442:
2413:BG Geminorum
2379:
2355:
2350:brown dwarfs
2274:
2254:circumbinary
2238:
2225:
2221:
2217:NN Serpentis
2205:Gamma Cephei
2193:PSR B1620-26
2182:
2177:protoplanets
2162:
2126:
2111:
2076:
2056:eccentricity
2049:
2045:stellar mass
2043:function of
2029:star systems
2026:
1842:Multiplicity
1829:population I
1761:
1747:
1727:
1723:
1716:
1711:
1704:
1696:
1694:
1681:
1674:
1668:
1663:
1542:
1540:is given by
1530:
1528:
1511:
1503:
1500:Astrophysics
1475:
1443:
1435:
1388:
1382:
1378:stellar wind
1374:
1346:
1334:
1306:
1194:
1189:
1185:
1183:
1180:Hot and cold
1169:
1167:
1149:
1145:
1141:
1137:
1133:
1129:
1125:
1123:
1104:Designations
1098:
1090:
1063:AM CVn stars
1057:
1033:stellar wind
1013:neutron star
989:neutron star
978:
945:
931:
929:
915:
914:
897:
896:
893:
868:Semidetached
822:
806:
801:
790:
786:neutron star
773:
771:
750:
721:
710:
694:
657:
655:
646:
641:
637:
632:
628:
623:
619:
614:
610:eccentricity
594:
590:
577:
566:spectrometer
555:
540:
502:
493:
482:Please help
477:verification
474:
441:
422:
417:
411:
407:
403:
401:
381:
379:
349:
323:
319:
309:
307:
294:
282:
280:
275:
265:
263:
247:
239:Félix Savary
225:
215:John Michell
212:
168:Double stars
166:
125:
123:
118:
114:
102:
94:
91:spectroscopy
86:
62:
58:
56:
6760:Outer space
6748:Spaceflight
6671:Double star
6614:Binary star
6609:Star system
6414:Brown dwarf
6190:Circumpolar
6068:Kraft break
6048:Color index
6023:Metallicity
5983:Designation
5952:Cosmic dust
5874:Photosphere
5640:Dark-energy
5615:Electroweak
5600:Black dwarf
5531:Radio-quiet
5514:White dwarf
5400:White dwarf
5050:Bok globule
4667:(6): 1657.
4296:(2): L133.
3826:: 252–283.
3618:: 621–629.
3365:Nguyen, Q.
3085:Bruton, D.
3061:Herter, T.
2732:: 339–382.
2522:107 Aquarii
2516:104 Aquarii
2503:Alcor–Mizar
2409:white dwarf
2405:Canis Minor
2332:white dwarf
2316:Canis Major
2209:white dwarf
2185:white dwarf
1954:1.5–5
1854:≤ 0.1
1849:companions
1839:Mass range
1490:Tycho Brahe
1446:white dwarf
1387:led to the
1242:white dwarf
1220:Eta Carinae
985:white dwarf
938:Roche lobes
809:astrometric
713:light curve
697:light curve
311:double star
283:binary star
59:binary star
51:white dwarf
6793:Star types
6782:Categories
6681:Star cloud
6376:Candidates
6371:Supernovae
6356:Red dwarfs
6215:Extinction
6003:Kinematics
5998:Luminosity
5976:Properties
5869:Atmosphere
5767:Si burning
5757:Ne burning
5695:White hole
5668:Quasi-star
5595:Blue dwarf
5450:Technetium
5366:Hypergiant
5344:Supergiant
4832:1811.00549
4797:2010-01-01
4775:Cygnus X-1
4584:: 219.05.
4229:1702.06160
4077:2006-06-25
3115:PowerPoint
3104:Worth, M.
2371:Beta Lyrae
2318:. In 1844
2298:. It is a
2296:black hole
2288:Cygnus X-1
2249:biospheres
2207:, and the
2139:luminosity
2087:giant star
2079:brightness
2003:≥ 16
1979:8–16
1844:frequency
1762:barycenter
1744:Barycenter
1712:barycenter
1538:barycenter
1450:Roche lobe
1411:Roche lobe
1357:Roche lobe
1330:protostars
1208:, such as
1195:Examples:
1119:AR Scorpii
1067:Beta Lyrae
1044:Cygnus X-1
1029:early-type
1017:black hole
993:black hole
983:such as a
902:Roche lobe
762:photometry
606:elliptical
582:telescopes
408:secondary.
392:binoculars
188:Ursa Major
184:Big Dipper
145:black hole
141:Cygnus X-1
99:astrometry
6736:Astronomy
6307:Brightest
6205:Magnitude
6185:Pole star
6106:Symbiotic
6101:Eclipsing
6033:Starlight
5834:Structure
5824:Supernova
5817:Micronova
5812:Recurrent
5797:Symbiotic
5782:p-process
5777:r-process
5772:s-process
5762:O burning
5752:C burning
5732:CNO cycle
5675:Gravastar
5211:Hypernova
5201:Supernova
5176:Dredge-up
5149:Blue loop
5142:super-AGB
5125:Red clump
5102:Evolution
5060:Protostar
5040:Accretion
5032:Formation
4825:(2): 98.
4736:0902.2179
4674:1010.4048
4621:0705.3444
4534:118982836
4465:119275313
4440:1303.3028
4256:119073723
3981:1001.4539
3950:118578253
3925:1001.3420
3893:119350572
3677:125947929
3591:22 August
3543:0707.3525
3405:0705.3444
3279:Bock, D.
3266:118394510
3249:1410.3074
3242:: 06063.
3199:CiteSeerX
3179:: 79–87.
2971:D. Reidel
2754:109971828
2478:Centaurus
2425:Milky Way
2423:" of the
2421:thin disk
2346:Luhman 16
2245:Nightfall
2240:Star Wars
2213:red dwarf
2201:red dwarf
2033:Milky Way
1566:⋅
1482:supernova
1467:CNO cycle
1353:evolution
1303:Formation
1277:Evolution
1210:R Aquarii
1037:late-type
1025:high-mass
496:July 2012
388:telescope
264:The term
260:Etymology
206:, in the
172:telescope
163:Discovery
133:evolution
83:telescope
73:that are
6686:Asterism
6486:Category
6381:Remnants
6277:Extremes
6237:Parallax
6210:Apparent
6200:Asterism
6178:Sunlight
6128:Globular
6113:Multiple
6038:Variable
6028:Rotation
5988:Dynamics
5879:Starspot
5553:Magnetar
5496:Remnants
5312:Subgiant
5285:Subdwarf
5137:post-AGB
4961:Archived
4912:14394432
4859:54511945
4792:BBC News
4699:59585356
4006:15893663
3787:Archived
3764:Archived
3432:14768050
3338:15301393
3221:18827791
3046:(1964).
2822:Archived
2799:Archived
2640:Archived
2621:Archived
2553:HD 30453
2509:See also
2382:61 Cygni
2260:Examples
2235:Tatooine
2197:subgiant
2137:, size,
2102:LTT 1445
2008:☉
1984:☉
1959:☉
1928:☉
1897:☉
1860:☉
1687:are the
1431:V Hydrae
1403:subgiant
1021:low-mass
944:forms a
854:Detached
666:parallax
662:eclipses
598:circular
416:(plural
287:resolved
235:orbiting
231:parallax
220:Pleiades
6722:Portals
6628:Unbound
6543:systems
6540:Stellar
6453:Gravity
6402:Related
6322:Nearest
6270:Chinese
6118:Cluster
6091:Contact
5928:Proplyd
5802:Remnant
5690:Blitzar
5664:Hawking
5620:Strange
5570:Burster
5526:Neutron
5479:Extreme
5430:He-weak
5075:T Tauri
4892:Bibcode
4837:Bibcode
4761:9893376
4741:Bibcode
4679:Bibcode
4626:Bibcode
4614:: 201.
4586:Bibcode
4514:Bibcode
4445:Bibcode
4387:Bibcode
4328:6725343
4308:Bibcode
4234:Bibcode
4160:Bibcode
3986:Bibcode
3930:Bibcode
3873:Bibcode
3828:Bibcode
3657:Bibcode
3620:Bibcode
3568:7759638
3548:Bibcode
3492:2590482
3472:Bibcode
3410:Bibcode
3318:Bibcode
3191:Bibcode
3144:Bibcode
2875:Bibcode
2779:Bibcode
2469:al-ghūl
2453:Perseus
2401:Procyon
2277:Albireo
2270:Albireo
2231:planets
2215:binary
2203:binary
2191:binary
2145:Planets
2135:density
2031:in the
1847:Average
1813:ellipse
1486:SN 1572
1454:accrete
1266:8823868
1258:KOI-81b
1250:6889235
1238:KOI-74b
1200:Antares
1109:A and B
1073:around
997:accrete
882:Contact
794:parsecs
533:in the
527:Algol A
525:orbits
523:Algol B
434:ellipse
418:comites
404:primary
200:Galileo
111:transit
107:eclipse
69:of two
6557:Galaxy
6443:Galaxy
6431:Planet
6419:Desert
6327:bright
6265:Arabic
6086:Binary
5906:Bubble
5630:Planck
5605:Exotic
5541:Binary
5536:Pulsar
5474:Helium
5435:Barium
5378:Carbon
5371:Yellow
5359:Yellow
5332:Yellow
5171:PG1159
4953:Curlie
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2498:Gemini
2494:Castor
2461:Arabic
2386:Cygnus
2362:Auriga
2308:Sirius
2284:Cygnus
2195:, the
2189:pulsar
2012:≥ 80%
1989:≥ 60%
1964:≥ 50%
1834:stars
1714:, and
1689:masses
1664:where
1492:. The
1264:
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814:Kepler
802:wobbly
739:, and
704:(i.e.
394:. The
266:binary
139:, and
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6550:Bound
6448:Guest
6252:Lists
6133:Super
5787:Fusor
5660:Black
5645:Quark
5625:Preon
5610:Boson
5546:X-ray
5462:Shell
5415:Ap/Bp
5317:Giant
5235:Early
5181:OH/IR
5011:Stars
4908:S2CID
4882:arXiv
4855:S2CID
4827:arXiv
4757:S2CID
4731:arXiv
4717:(PDF)
4695:S2CID
4669:arXiv
4616:arXiv
4530:S2CID
4504:arXiv
4461:S2CID
4435:arXiv
4377:arXiv
4324:S2CID
4298:arXiv
4252:S2CID
4224:arXiv
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1015:or a
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180:Acrux
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6018:Mass
5842:Core
5792:Nova
5685:Iron
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5322:Blue
5240:Late
5022:List
4403:ISBN
4191:ISBN
4097:ISBN
4043:ISBN
3744:ISBN
3702:ISBN
3593:2008
3586:NASA
3010:ISBN
2979:ISBN
2927:ISBN
2704:ISBN
2673:ISBN
2375:Lyra
2130:sine
2104:, a
2020:0.20
2016:1.30
1997:0.20
1993:1.00
1972:0.10
1968:1.00
1947:0.03
1943:0.62
1916:0.05
1912:0.33
1878:0.22
1680:and
1471:nova
1230:NASA
1215:The
1128:and
818:laws
778:mass
602:sine
423:The
198:and
178:and
155:and
109:and
6424:Sub
6158:Sun
5577:SGR
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4951:at
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4878:660
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3859:633
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3396:342
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2923:1–2
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