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implementation in digital electronic circuitry using logic gates, the binary system is used by almost all modern computers and computer-based devices, as

HU Aquarii (abbreviated HU Aqr) is an eclipsing binary system approximately 620 light-years away from the Sun, forming a cataclysmic variable of AM Herculis-type

circumbinary exoplanet in the binary-star system Kepler-453. It orbits the binary system in the habitable zone every 240.5 days. The orbit of the planet is inclined

its minor-planet moon are similar in mass and size, making it a true binary system. The components are estimated to measure 1.8 kilometers in diameter

high-resolution imaging resolved the star Kepler-14 as a closely orbiting binary system. The Kepler team would have not noticed that Kepler-14 was a binary

spectroscopic binary system with a close circular orbit taking just 0.945 days to complete. Despite their proximity, this does not appear to be a contact binary system

orbits two stars instead of one. The two stars orbit each other in a binary system, while the planet typically orbits farther from the center of the system

LS I +61 303 is a binary system containing a massive star and a compact object. The compact object is a pulsar and the system is around 7,000 light-years

oxygen-rich Wolf–Rayet star. An analysis of Gaia data suggests that it is a binary system. "Search results for NGC 7026". Astronomical Database. SIMBAD. Retrieved

analysis of Gaia data suggests that the central star may be a binary system. A binary system could explain the abundance discrepancy. While on the cooling

QS Virginis (abbreviated QS Vir) is an eclipsing binary system approximately 163 light-years away from the Sun, forming a cataclysmic variable. The system

1783 by William Herschel from his home in Slough England. It is a binary system together with the bright spiral galaxy M77 (NGC 1068). These two are

approximately 2,700 astronomical units, an unusually wide separation for a binary system. Double star Binary star List of NGC objects (1–999) Seligman, Courtney

Despite their proximity to each other, this does not form an eclipsing binary system because the inclination of the orbital plane to the line of sight to

single-lined spectroscopic binary system with a period of 1.92 hours in a close, circular orbit. The pair form an eclipsing binary system that decreases from

NASA/ESA Hubble Space Telescope's Faint Object Camera in 1994. The binary system consists of two red dwarfs orbiting each other at a distance of 1.9

magnitude. An analysis of Gaia data suggests that the central star is a binary system. Distance is estimated at 1.7 kpc. Kerber, F.; et al. (September 2003)

program. This is probably a binary system with an unseen companion. It is physically associated with the likely binary system HIP 19255, with the two pairs

distance of around 8 kiloparsecs (26,000 light-years). The lens star is a binary system approximately 10,000 light-years away in the constellation Sagittarius

HR 273 is a chemically peculiar spectroscopic binary system in the northern circumpolar constellation of Cassiopeia. It has an apparent visual magnitude

XTE J1650−500 is a binary system containing a stellar-mass black hole candidate and 2000–2001 transient binary X-ray source located in the constellation

HD 3443 is a binary system composed of medium-mass main sequence stars in the constellation of Cetus about 50 light years away. This binary star system

In astronomy, the Roche lobe is the region around a star in a binary system within which orbiting material is gravitationally bound to that star. It is

in the sky since Kepler's Supernova in 1604. Like all novae, it is a binary system, comprising a white dwarf and donor low-mass star in close orbit to

HD 20781 is a star which is part of a wide binary system with HD 20782. The companion star has a very large angular separation of 252 arcsec, corresponding

ratio of the two components – called the "primary" and "secondary" of a binary system – is an important characteristic. Most binary asteroids have a large

heliocentric radial velocity of −33 km/s. This is a single-lined spectroscopic binary system with an orbital period of 576 days and an eccentricity of 0.3. The a

M33 X-7 is a black hole binary system in the Triangulum Galaxy. The system is made up of a stellar-mass black hole and a companion star. The black hole

system in the constellation of Taurus 450 light-years from Earth. The binary system itself is known as L1551 NE, and each star is surrounded by protoplanetary

GK Tauri is a young binary system composed of T Tauri-type pre-main sequence stars in the constellation of Taurus about 466 light years away, belonging

relatively high luminosity for a standard white dwarf. It is also in a close binary system with orbital period of 1.4933 days. Brown, A. G. A.; et al. (Gaia collaboration)

important. An analysis of Gaia data suggests that the central star is a binary system. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data

velocity of −5 km/s. Sigma Aquilae is a double-lined spectroscopic binary system consisting of two intermediate-mass B-type main sequence stars; each

a visual binary system with the components separated by 0.6″ and a combined spectral class of O8. One of stars is an eclipsing binary system. The period

lasting only for about 1 ms. Cygnus X-1 belongs to a high-mass X-ray binary system, located about 7,000 light-years away, that includes a blue supergiant

star systems; one more is suspected. HD 205117 is a probable eclipsing binary system with a period of 113.2 days that varies by 0.051 in visual magnitude

giant stars. The brightest member of the cluster is DL Cassiopeiae, a binary system which contains a Cepheid variable with a 8,00 day period. Using the

star believed to contain a white dwarf and a Mira-type variable in a binary system. The orbital period is approximately 44 years. The main Mira-type star

near-infrared counterpart was determined by spectroscopic observations. The binary system lies 11,000 parsecs away in Aquila. The black hole in GRS 1915+105 is

HD 213429 is a spectroscopic binary system in the equatorial constellation of Aquarius. It has a combined apparent magnitude of 6.16 and is located around

most likely forms a gravitationally bound pair with the magnitude 5.45 binary system KT Vel (HD 74535); both are members of the IC 2391 open cluster. As

constellation of Auriga, the charioteer. It is an unusual eclipsing binary system comprising an F0 supergiant (officially named Almaaz /ælˈmɑːz/, the

located about 1,250 light-years away in the Andromeda constellation. The binary system consists of a metal-rich F-type main-sequence star, named WASP-1A, and

78+101123.3 (shortened to SDSS J1433+1011, more simply J1433) is a binary system composed of a white dwarf and a brown dwarf. The brown dwarf is about

constellation of Aquila. Two of the components form a close spectroscopic binary system, while a third star, also thought to be a spectroscopic binary, orbits

type of O(H)3 III-V. An analysis of Gaia data suggests that it is a binary system. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data

to translate logical reasoning into pure mathematics. He viewed the binary system as a means of simplifying complex logical and mathematical processes

light-years from Earth in the constellation Sagittarius. It is part of a binary system and undergoes regular eclipses with an eclipse magnitude of about 40%

stars by W. Strohmeierand and associates in 1965, demonstrating it is a binary system with an orbital inclination close to the line of sight from the Earth

a dwarf nova. After the eruption of 1919, the orbital period of the binary system has decreased by 0.0273±0.0061%, to the 5.786290±0.000032 days. Physical

HW Virginis, abbreviated HW Vir, is an eclipsing binary system (of the Algol type), approximately 563 light-years away based on the parallax measured

inner pair, designated component A, has been described as an eclipsing binary system, showing a primary minimum of 6.05 and a secondary minimum of 6.04.

5 ly some 3.12 million years ago. This is a double-lined spectroscopic binary system, having a circular orbit with a period of 2.5 days. It was discovered

light-years away in the constellation of Sculptor, orbiting a star in the binary system HD 4113 A. This planet has a very eccentric orbit with a 527-day period

William Herschel. NGC 7332 and NGC 7339 form a dynamically isolated binary system (number 570 in the catalog of double galaxies compiled by Igor Karachentsev)

northern constellation of Perseus, abbreviated RT Per. It is an eclipsing binary system with an orbital period of 0.84940032 d (20.386 h). At peak brightness

minutes, which makes the determination of the orbital period of the binary system comprising the nova difficult. The orbital period may be 0.136±0.002

telescopes. This occurs because the pair either forms a binary star (i.e. a binary system of stars in mutual orbit, gravitationally bound to each other) or is

stars are more likely to produce non-spherical nebulae. For LoTr 5, the binary system likely played a role in shaping the nebula. A modelling of LoTr 5 shows

Chi Draconis (χ Dra, χ Draconis, Chi Draconis) is a magnitude 3.6 binary star in the constellation Draco. It also has the Flamsteed designation 44 Draconis

David Dunlap Observatory in 1945. This is a double-lined spectroscopic binary system with an orbital period of 11 days and an eccentricity of 0.19. The two

yielding a separation of 291 light years. This is a detached eclipsing binary system of the Beta Lyrae type. The orbital period for the system is 1.5755 days

measuring changes in the spectrum of the primary. The orbital period of the binary system is 4197.7 days (11.5 years). The primary component has a stellar classification

heliocentric radial velocity of 12 km/s. This is a double-lined spectroscopic binary system with an orbital period of 36 days and an eccentricity of 0.543. The

companion is a hotter, A- or B-type star that is a suspected spectroscopic binary system. The visible pair have an angular separation of 1.71 arcseconds. Vallenari

Jr. and Russell Hulse discovered for the first time a pulsar in a binary system of stars, PSR B1913+16. This pulsar orbits another neutron star with

system which features a neutron star and a low-mass companion star. The binary system lies 10,000 light-years away in Orion. It produces jets like a microquasar

designation 1997 CS29) is a cold classical Kuiper belt object (cubewano) and binary system made up of components of almost equal size, called Sila and Nunam, orbiting

range, while the outer tertiary takes 70000 years to orbit the inner binary system. Due to their proximity and the intense gravity of the black hole, the

M. T.; Bisikalo, D. V. (2007). "Bipolar ejection by the symbiotic binary system Z and during its 2006 outburst". Mon. Not. R. Astron. Soc. 376 (1):

latter) and represents the number one hundred, while (100)2 (in the binary system with base 2) represents the number four. Radix is a Latin word for "root"

often referred to as a pinwheel nebula. The rotational axis of the binary system, and likely of the two closest stars, is directed approximately towards

spectrum of 57 Peg displays blended features that indicate this is a binary system consisting of an aging red giant star on the asymptotic giant branch

Rügemer and H. Schneller independently discovered this is an eclipsing binary system of the Algol type. Rügemer later found that the eclipse period was not

carbon-type Wolf–Rayet (WR) star and in 1945 was found to be a spectroscopic binary system by W. A. Hiltner. This system was reported to be an eclipsing binary

thus, Salacia and Actaea are viewed by William Grundy et al. to be a binary system. Assuming that the following size estimates are correct, Actaea is about

calculated to be 85.3 million years. It includes one known spectroscopic binary system. An interesting feature of M26 is a region of low star density near

both surrounded by ejected material. HR Carinae is also likely to be a binary system with a similar separation, period, and ratio of component sizes to Eta

physically associated with ζ1 Lyrae. This is a single-lined spectroscopic binary system with an orbital period of 4.3 days and a nearly circular orbit with

HR 2554, also known as V415 Carinae and A Carinae, is an eclipsing spectroscopic binary of the Algol type in the constellation of Carina whose apparent

parallax measurements, is roughly 380 light years. This is a spectroscopic binary system with a stellar classification of A5V. They have an orbital period of

Nina A. (2013). "Analysis of the motion of an extrasolar planet in a binary system". The Astronomical Journal. 146 (5): 108. arXiv:1212.3843. Bibcode:2013AJ

Serpentis (abbreviated NN Ser) is an eclipsing post-common envelope binary system approximately 1670 light-years away. The system comprises an eclipsing

enriched with s-process elements. It is either a member of a close binary system and has previously acquired these elements from a (now) white dwarf

fast nova with a smooth light curve. Like all novae, V382 Velorum is a binary system with two stars orbiting so close to each other that one star, the "donor"

measured changes in the star's motion, this is most likely an astrometric binary system. The visible component is an A-type main-sequence star with a stellar

(provisional designation 2013 FY27) is a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced

proper motion and radial velocity it is likely that the two constitute a binary system. On 21 December 2010 it was occulted by the Moon during a Total Lunar

NSVS 14256825, also known as V1828 Aquilae, is an eclipsing binary system (of the Algol type) in the constellation of Aquila. The system comprises a subdwarf

radial velocity of this star suggest it is a single-lined spectroscopic binary system. This yields orbital elements with a period of 48.3 days and an eccentricity

constellation Cygnus, approximately 69 light years away from Earth. This visual binary system has a period of 49.6 years. The main star, 4th magnitude GJ 822.1 A

to rule out a white dwarf companion, so it may instead itself be a binary system consisting of two smaller stars having an orbital period between a week

with a regular period of 2.2475 days due to distorted stars in a close binary system composed by an O3 class giant and an approximately O5 class companion

discovery observation. In 2001, it was discovered that Patroclus is a binary system, made up of two components of roughly similar size. It is one of six

and seems to be at the same distance, confirming they form a physical binary system. In 2005, an exoplanet was discovered around HD 109749 A. It was detected

FU Tauri is a brown dwarf binary system in the constellation of Taurus about 429 light years away. The secondary is very close to the lower limit for

heliocentric radial velocity of −3 km/s. This is a single-lined spectroscopic binary system with an orbital period of 2.58 years and an eccentricity of 0.4. The

393 light years from the Sun. This is a single-lined spectroscopic binary system with a nearly circular orbit and a period of 7.45 years. The fact that

exoplanet orbiting a red dwarf, later studies determined that KOI-256 was a binary system composed of the red dwarf orbiting a white dwarf. The acronym "KOI"

supernova discovery. This single-degenerate white dwarf with normal star binary system represents one of two mechanisms for producing a type-Ia supernova,

over time suggests some displacement, which may indicate it is a close binary system. This is an aging giant star with a stellar classification of K5 III

(DM Lyr for short) is a dwarf nova in the constellation Lyra. This binary system is composed of a primary star of unknown type, and a white dwarf companion

due to an acceleration component, which may indicate it is a close binary system. The visible component has a stellar classification of G5 V, indicating

Radial velocity studies indicate that the star may be a member of a binary system. The nebula does not show enrichment of s-process elements. This suggests

RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away, belonging to the Taurus-Auriga association of the Taurus

velocity of +2 km/s. This is a candidate double-lined spectroscopic binary system. It has a stellar classification of A1V, suggesting the primary component

center of the galaxy. It is possible that it was originally part of a binary system that was tidally disrupted by the supermassive black hole, causing it

Mount Wilson observatory in 1952. It is a double-lined spectroscopic binary system with an orbital period of 1.581 years and an eccentricity of 0.24. Both

star is the Andromeda Galaxy. Nu Andromedae is close spectroscopic binary system with a period of 4.2828 days and a nearly circular orbit. The primary

RV Tauri (RV Tau) is a star in the constellation Taurus. It is a yellow supergiant and is the prototype of a class of pulsating variables known as RV Tauri

(provisional designation 2000 YW134) is a resonant trans-Neptunian object and binary system, located in the outermost region of the Solar System. It was discovered

caused by intervening gas and dust. This is a double star and possible binary system. The primary component has a stellar classification of G2 Ib/II, which

of the Sun. Indeed, it was long thought to be the most massive known binary system, but evidence collected between 1996 and 2005 demonstrated that Eta

radial velocity of +3.76 km/s. This is a double-lined spectroscopic binary system consisting of two similar components designated Aa and Ab. The initial

Theta Eridani, Latinized from θ Eridani, is a binary system in the constellation of Eridanus with a combined apparent magnitude of 2.88. Its two components

PSR J0348+0432 is a pulsar–white dwarf binary system in the constellation Taurus. It was discovered in 2007 with the National Radio Astronomy Observatory's

ROXs 12 is a binary system of pre-main-sequence stars. It belongs to the Rho Ophiuchi cloud complex. The surface temperature of the primary star is 3900±100

show changes in motion that may indicate it is a member of a close binary system. This is an A-type main-sequence star with a stellar classification

heliocentric radial velocity of 5 km/s. The primary component is a binary system consisting of two nearly equal components with an orbital period of

58534 Logos, or as a binary system (58534) Logos-Zoe, is a trans-Neptunian object and binary system from the classical Kuiper belt, approximately 77 kilometers

a companion; most likely a low-mass main sequence star. This close binary system has an orbital period of 1.47 hours, which is one of the shortest periods

69230 Hermes is a sub-kilometer sized asteroid and binary system on an eccentric orbit, classified as a potentially hazardous asteroid and near-Earth

CP2 variable to be discovered was α2 Canum Venaticorum, a star in the binary system of Cor Caroli, which lies in the northern constellation of Canes Venatici

it at a distance of about 860 light years (260 parsecs). This is a binary system with the two components separated by 0.446″. The secondary is nearly

low-mass red dwarfs with at least one of them being a flare star. This binary system has a circumbinary sub-stellar companion. This star was mentioned as

XZ Tauri is a binary system approximately 460 light-years away in the constellation Taurus. The system consists of two T Tauri stars orbiting each other

is an RS Canum Venaticorum variable system. This is a near-contact binary system with a circular orbit having a period of 19.61 hours. The orbital plane

America, a binary system of gender was enforced as a means of maintaining patriarchal norms and upholding European nationalism. The binary system has also

co-moving stars. The magnitude 5.3 primary component forms a near-contact binary system, with the components designated Aa and Ab. It has a combined class of

SS 433 is a microquasar or eclipsing X-ray binary system, consisting of a stellar-mass black hole accreting matter from an A-type companion star. SS 433

6 kpc according to its Gaia Data Release 2 parallax. The star in the binary system is a late B class giant with a mass about three times that of the Sun

away from the Sun at the rate of +2 km/s. This is a detached eclipsing binary system with the secondary eclipse being total. The pair are orbiting each other

XZ Tauri is a binary system approximately 460 light-years away in the constellation Taurus. The system consists of two T Tauri stars orbiting each other

a radial velocity of +24 km/s. This is a single-lined spectroscopic binary system with an orbital period of 2.46 years and an eccentricity of 0.12. The

each other at an average distance of 1,200 astronomical units. The binary system is listed as Struve 1341 in the Struve Catalogue of Double Stars; however

it at a distance of about 860 light years (260 parsecs). This is a binary system with the two components separated by 0.446″. The secondary is nearly

W. GCIRS 13E was initially modelled as a single object, possibly a binary system. It was even classified as a Wolf-Rayet star because of its strong emission

co-moving stars. The magnitude 5.3 primary component forms a near-contact binary system, with the components designated Aa and Ab. It has a combined class of

6.36 primary, component A, is actually a double-lined spectroscopic binary system with an orbital period of 12.822 days, an eccentricity of 0.39, and

(abbreviated SDSS J1416+1348 and nicknamed Rimmer) is a nearby wide binary system of two brown dwarfs, located in constellation Boötes. The system consists

Star of Heaven's Great General.) This is most likely a spectroscopic binary system with an estimated orbital period of 20.8 years and an eccentricity of

obscuring the light from the primary component. This is a semidetached binary system with an orbital period of 2.0563056 days in an essentially circular

However, Chini et al. (2012) listed it as a single-lined spectroscopic binary system. The visible component of V343 Carinae has a stellar classification

known pre-main-sequence star, meaning that the two may form a very wide binary system; if not, they are still in the same star association. van Leeuwen, F

discovered within 1 kpc of the Sun, namely BD+66 1673, which is an eclipsing binary system consisting of an O5V that exhibits a surface temperature of nearly 45

found to vary periodically and it was determined to be an eclipsing binary system—the third such discovered. The components of this system have a combined

earlier hypothesized by Alonso et al. (2008), making CoRoT-2 a wide binary system with at least one planet. This star is home to exoplanet CoRoT-2b discovered

a radial velocity of −34 km/s. This is a single-lined spectroscopic binary system with an orbital period of 32.0 years and a high eccentricity of 0.73

velocity of −10 km/s. At one point this was thought to be a spectroscopic binary system. It is a Be star with a weak circumstellar disk of gas that has around

when viewed in the night sky. This is a single-lined spectroscopic binary system, but the secondary has been detected using interferometry. It is an

AO Cassiopeiae, also known as Pearce's Star, is a binary system composed of an O8 main sequence star and an O9.2 bright giant that respectively weigh

Wolf–Rayet star. An analysis of Gaia data suggests that the it may be a binary system. The central star was monitored by the Kepler space telescope, but it

Thuban (/ˈθjuːbæn/), with Bayer designation Alpha Draconis or α Draconis, is a binary star system in the northern constellation of Draco. A relatively

390 light-years from the Sun. This is a single-lined spectroscopic binary system with an orbital period of 3.8 years and an eccentricity of 0.35. The

further papers in 2020 and one in 2022 concluded that HR 6819 is simply a binary system with two main-sequence stars and no black hole at all. HR 6819 is the

enriched with s-process elements. It is either a member of a close binary system and has previously acquired these elements from a (now) white dwarf

extinction caused by interstellar gas and dust. This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in

of the cluster lies DH Cephei, a close, double-lined spectroscopic binary system consisting of two massive O-type stars. This pair are the primary ionizing

related by interferometry to distant quasars. The two components of the binary system includes a K-type giant star and a G-type main sequence star. The primary

found variations in radial velocity over time that suggested this is a binary system. However, confirmation of this proved difficult because of the distance

heliocentric radial velocity of −2 km/s. This is a single-lined spectroscopic binary system with an orbital period of 363.57 days and an eccentricity of 0.35. The

within 49 light-years in half a million years. This is an astrometric binary system. The visible component is an ordinary F-type main-sequence star with

Based on radial velocity variations, it is a candidate spectroscopic binary system and a preliminary orbital solution was published in 1991 with a period

07 M☉. An analysis of Gaia data suggests that the central star may be a binary system. NGC 6905 can be detected under dark skies with a 4-inch telescope,

suggests it belongs to neither. This is a single-lined spectroscopic binary system with an orbital period of 81.5 days and a significant eccentricity of

PSR J1614–2230 is a pulsar in a binary system with a white dwarf in the constellation Scorpius. It was discovered in 2006 with the Parkes telescope in

it is too faint to be visible to the naked eye. This is an eclipsing binary system that decreases to magnitude 10.05 during the primary eclipse, then to

Gliese 829 is a double-lined spectroscopic binary system of two red dwarf stars in the constellation of Pegasus. They have a high proper motion of 1.08 arc

and an F-type main sequence star. Two of the stars form an eclipsing binary system and revolve around each other once every 7.15 days. These in turn orbit

Tauri is the Bayer designation. This is a single-lined spectroscopic binary system with the two components orbiting each other over a period of 4.53 years

spot" hypothesis was proposed to explain this feature. This is a close binary system with an orbital period of 15.4 hours. It is classified as a W Ursae

2 hours and 57 minutes, which is probably the orbital period of the binary system. In addition, brightness variations with a period of 22 minutes are

time scale as low as a few hours. They interpreted this as a detached binary system consisting of a compact, high temperature white dwarf and a cool red

radial velocity of 16.65 km/s. This is a double-lined spectroscopic binary system with an essentially circular orbit and a period of one week. The primary

radial velocity of 16.65 km/s. This is a double-lined spectroscopic binary system with an essentially circular orbit and a period of one week. The primary

three-light-year margin of error. This is a single-lined spectroscopic binary system, meaning that the presence of an orbiting companion is revealed through

a radial velocity of +10 km/s. This is a single-lined spectroscopic binary system with an orbital period of 28.7 years and an eccentricity of 0.65. The

approximately 115 light-years (35 parsecs) from Earth. This is an astrometric binary system. The visible component is an F-type main sequence star with a stellar

Tauri is the Bayer designation. This is a single-lined spectroscopic binary system with the two components orbiting each other over a period of 4.53 years

spot" hypothesis was proposed to explain this feature. This is a close binary system with an orbital period of 15.4 hours. It is classified as a W Ursae

Omega Eridani was long thought to be a is a single-lined spectroscopic binary system, with an orbital period of 3,057 days (8.4 years) and an eccentricity

equivalent to approximately ten million Suns. This object is part of a binary system: If the pulsar is of an average size, 1.4 M☉, then its companion is

of 380 light-years (120 parsecs) from Earth. This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in

has been derived from fitting the spectrum. 26 Aurigae is a visual binary system, and the two stars orbit each other every 52.735 years with an ellipticity

radial velocity of +6.5 km/s. ζ Cen is a double-lined spectroscopic binary system, which indicates that the orbital motion was detected by shifts in the

long been a white dwarf. Depending on the initial properties of the binary system, the polluted star can be found at different evolutionary stages. During

Goran et al. (1991) NGC 1333 IRAS 4 – A very young, low-luminosity binary system SpaceDaily: NASA's Spitzer Digs Up Troves of Possible Solar Systems

apparent visual magnitude of 4.64. This is a single-lined spectroscopic binary system, with the presence of a companion being demonstrated by shifts in the

object, or planemo. The system was announced as the first reported binary system of objects this small. However, later observations and calculations

photosphere at an effective temperature of 5,718 K. In 2008 a co-moving binary system of low mass companions were discovered at an angular separation of 7″

eccentricity of 0.536. The magnitude 6.02 primary, component A, is itself a binary system consisting of two stars of similar mass, roughly 1.5 times the mass

Beta Leonis Minoris, Latinized from β Leonis Minoris, is a binary star in the constellation of Leo Minor. It has an overall apparent visual magnitude of

1991 VL) is a highly eccentric, rare-type asteroid and synchronous binary system, classified as near-Earth object of the Apollo group, approximately

solar masses and 20 times the radius of the Sun. The period of the binary system is 5.8 days and the pair is separated by 0.2 astronomical units. The

give or take a 30 light-year margin of error. This is an astrometric binary system. The primary has a stellar classification of F2 III, suggesting that

equipment, stars can be resolved at closer distances. For a visual binary system, measurements taken need to specify, in arc-seconds, the apparent angular

A binary opposition (also binary system) is a pair of related terms or concepts that are opposite in meaning. Binary opposition is the system of language

around 293 light years. Tau5 Eridani is a double-lined spectroscopic binary system. The two stars orbit each other closely with a period of 6.2 days and

thought that this is due to the viewpoint of looking directly down on a binary system whose orbit is perpendicular to Earth. Discovered in 1936 by Harlow

Telescopii (HR 6819), however observations in 2022 indicated that this is a binary system of two main-sequence stars without a black hole instead. Telescopium

Struve computed the orbital elements for a single-lined spectroscopic binary system with a short orbital period of just 17 hours. He found a stellar classification

radial velocity of +4.5 km/s. φ Cygni is a double-lined spectroscopic binary system, which means that the absorption lines of both components are visible

Arietis system contains three stars. The inner pair form an eclipsing binary system, with the brightness of the pair decreasing by 0.06 in magnitude during

observed in 1973 and 1974–5. It is actually a confirmed spectroscopic binary system with a high temperature subdwarf O-type companion in a 28-day orbital

metallic-line Am star. It is a white-hued, single-lined spectroscopic binary system, located about 127 light-years from Earth. The pair have an orbital

brightness variations of a few tenths of a magnitude. Each component of the binary system is slightly under 3 M☉. Although they have a subgiant spectral classification

findings announced in 1955. It was found to be a detached eclipsing binary system, and by 1963 a variable primary component had been noted. E. H. Geyer

MSPs are neutron stars that have been spun up by accretion in a close binary system. The change in rotational period of the neutron star comes from the

speed is caused by the transfer of material from a companion star in a binary system. After this "cosmic dance", the donor star is predicted to explode as

radar astronomers at Goldstone Observatory. The primary body of the binary system has a rotation period of 3.3 hours, while the secondary's orbital period

Located at an estimated distance of 3.8 kly (1.17 kpc), this is a close binary system with a degenerate white dwarf primary in orbit with a cool red dwarf

observations revealed an orbital period of 4.52138±0.00012 hours for the binary system. "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021. Brown

a visually moderately bright Wolf-Rayet star. It is a spectroscopic binary system containing a Wolf-Rayet primary and a class O supergiant secondary.

J082303.1-491201 (also known as DENIS J082303.1-491201, DE0823-49), is a binary system of two brown dwarfs, located 20.77 parsecs (67.7 ly) from Earth. The

observations revealed an orbital period of 4.52138±0.00012 hours for the binary system. "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021. Brown

findings announced in 1955. It was found to be a detached eclipsing binary system, and by 1963 a variable primary component had been noted. E. H. Geyer

in 2011. It was unclear whether the pair formed a visual double or a binary system. The authors of the study estimated a class of K2 V, based upon a visual

plausible model suggests the progenitor was part of an interacting binary system where much of the atmosphere was lost through mass transfer to the companion

to observe. However, NGTS-3 is actually an unresolved spectroscopic binary system. The system is located approximately 2,480 light years away, based on

(357439) 2004 BL86 is a bright sub-kilometer asteroid and binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo

Gordon published orbital elements for this single-lined spectroscopic binary system in 1946, giving an orbital period of 4.29 years and an eccentricity

constellation boundary with Pisces. This is a probable astrometric binary system, as determined by changes to the proper motion of the visible component

around 643,000 years. This appears to be a single-lined spectroscopic binary system with an orbital period of 130.7 days and an eccentricity of 0.366. It

value of roughly 327 light years. This is a double-lined spectroscopic binary system with an orbital period of 5.95382 days and an eccentricity of 0.12.

the group, designated component A, is a single-lined spectroscopic binary system with a circular orbit and a period of 3.88 days. The visible component

amorphous carbon. László Szabados suggested in 1990 that this might be a binary system with a period of 507 days. A detection of this projected companion was

other star in the system. Gliese 268 in particular is composed of a binary system of two M-type dwarfs, or red dwarfs, and is one of the one hundred closest

a heliocentric radial velocity of roughly −10 km/s. This is a wide binary system with an orbital period of 228 years and an eccentricity of 0.80. As

images found back in 2012. The potentially hazardous asteroid is a binary system with a minor-planet moon in its orbit. The discovery was made by astronomers

in distance of ±10 light years. This is a single-lined spectroscopic binary system, which means that the two stellar components have not been individually

Gliese 676 is a 10th-magnitude wide binary system of red dwarfs that has an estimated minimum separation of 800 AU with an orbital period of greater than

magnitudes brighter than expected. This may indicate that this is a binary system with an unresolved secondary component. It has 15% more mass than the

IRAS 16293–2422 is a binary system consisting of at least two forming protostars A and B, separated by a distance of 700 astronomical units (au), both

motion with the magnitude 6.06 star HD 92463, and the pair likely form a binary system. This secondary component is a B-type main-sequence star with a class

designated Zeta Sculptoris A, is a single-lined, low amplitude spectroscopic binary system with an orbital period of 4.8 years and an eccentricity of 0.32. The

Tucanae displays strong oscillations, suggesting this is a spectroscopic binary system. A companion was directly detected in 2014, but this result has some

are receding with a radial velocity of +2.6 km/s. This is a visual binary system with the components orbiting each other over a period of roughly 700 years

drifting nearer with a radial velocity of −26 km/s. This is a wide binary system with a computed orbital period of 217 years and an eccentricity of 0

internal dynamics of the hot B subdwarf component in the close eclipsing binary system PG 1336-018". Astronomy and Astrophysics. 489 (1): 377. Bibcode:2008A&A

that its mass is around 1.4 M☉, deduced from the mass ratio of the binary system and the modelled mass of the primary star. The primary itself is calculated

velocity of -33 km/s. The double-lined nature of this spectroscopic binary system was not announced until 1972. It has an orbital period of 1.35 years

Eri or α Eri. The name Achernar applies to the primary component of a binary system. The two components are designated Alpha Eridani A (the primary) and

5 arcseconds away with the same proper motion, indicating a stellar binary system. The binarity was confirmed in 2020. The axis orientation of the primary

X Persei is a high-mass X-ray binary system located in the constellation Perseus, approximately 950 parsecs away. It is catalogued as 4U 0352+309 in the

merger event of two smaller black holes. As of June 2020[update], the binary system 2MASS J05215658+4359220 was reported to host the smallest-mass black

It is a very active RS Canum Venaticorum variable (RS CVn), a close binary system with active starspots. The primary (II Pegasi A) is a cool subgiant

PSR J0740+6620 is a neutron star in a binary system with a white dwarf, located 4,600 light years away in the Milky Way galaxy. It was discovered in 2019

long-term cyclical variation of changing amplitude and period. The modelled binary system shows a primary with a class of around B5–7e and a low mass secondary

to the determination that 15 Cancri is a single-lined spectroscopic binary system. The first orbit was calculated in 1973 by Helmut Abt and Michael Snowden

10 light-years (3.1 parsecs). This is a single-lined spectroscopic binary system with an orbital period of 2.8 years and an eccentricity of 0.1. The

K2-288Bb has a close orbit around the second, smaller star of the binary system. It orbits every 31.393 days at a distance of about 0.164 AU. For comparison

+9 km/s. Based upon proper motion variation, this is an astrometric binary system with high likelihood (99.8%). The visible component has a stellar classification

apparent visual magnitude of +6.02. It is a single-lined spectroscopic binary system with an orbital period of 6.63 years and a high eccentricity of about

variations which are, in general, close to the orbital period of the binary system. Some systems exhibit variations in luminosity due to their being eclipsing

main-sequence star with a stellar classification of A0Va. It may form a binary system of two roughly equal stars. An infrared excess suggests there is a debris

light-years (113 parsecs) from Earth. Sigma Piscium is a spectroscopic binary system, meaning the components of the system have been detected from periodic

17.5 kpc away from the Galactic Center. This star was found to be a binary system based on variations in radial velocity data collected from the Hipparcos

with a radial velocity of +16 km/s. This is listed as an eclipsing binary system with a period of 47.9 days (although the star does not appear to be

GS 2000+25 is an X-ray binary system in the constellation Vulpecula, consisting of a late K-type star and a black hole. It is also an X-ray nova. Fumiyoshi

away, in the constellation Cepheus. Component A is a spectroscopic binary system with an orbital period of 7.753 days and a combined stellar classification

star system. Analysis of its spectrum shows that it is a spectroscopic binary system with the fainter companion calculated to be a main sequence star of

moon of the near-Earth asteroid 65803 Didymos, with which it forms a binary system. The moon was discovered on 20 November 2003 by Petr Pravec in collaboration

it is too old to be a member. This star was identified as a visual binary system by G. W. Hough in 1844 and given the identifier HO 212. The pair have

is understood that these flares are induced by a companion star in a binary system which causes the magnetic field to become tangled. Additionally, nine

is understood that these flares are induced by a companion star in a binary system which causes the magnetic field to become tangled. Additionally, nine

175 light years from the Sun. This is a double-lined spectroscopic binary system with an orbital period of nearly two days in a circular orbit. It is

Didymos (provisional designation 1996 GT) is a sub-kilometer asteroid and binary system that is classified as a potentially hazardous asteroid and near-Earth

Abt et al. (1969) determined this to be a single-lined spectroscopic binary system and computed an orbital solution with a period of 80.17 days and an

and extrinsic S stars, which are formed through mass transfer in a binary system. The intrinsic S-type stars are on the most luminous portion of the

roughly 640 light-years (196 parsecs) from Earth. This is a spectroscopic binary system, which means that the presence of an orbiting companion has been revealed

it is too old to be a member. This star was identified as a visual binary system by G. W. Hough in 1844 and given the identifier HO 212. The pair have

subject to lunar occultation. Xi Aquarii is a single-lined spectroscopic binary system, which means that the presence of an unseen orbiting companion can be

large space velocity, probably caused by being ejected from a close binary system when its companion exploded as a supernova. Zeta Puppis is typical of

mission and carries out observational analysis of the Didymos asteroid binary system after DART's impact on Dimorphos. It communicates directly with Earth

"recycled" through accretion of matter from a companion star in a close binary system. For this reason, millisecond pulsars are sometimes called recycled

radial velocity of −11.7 km/s. This is a double-lined spectroscopic binary system with an orbital period of 9.3 days and a small eccentricity of 0.0116

WR 140 is a visually moderately bright Wolf–Rayet star placed within the spectroscopic binary star, SBC9 1232, whose primary star is an evolved spectral

Batten et al. (1989) catalogued it as a double-lined spectroscopic binary system with an orbital period of four days and an eccentricity of 0.02. However

000 to 250,000 K. The hypothesis that the central star is actually a binary system is promising for this object. M1-92’s spectrum is rather complex. It

stellar companion of spectral class F8. This pair may form an eclipsing binary system with a period of 785 days (2.15 years), resulting in a magnitude change

system is roughly 520 light years. This is a single-lined spectroscopic binary system, which means that only the absorption line features of one of the components

variations with a period of 4.32 days. There is little doubt that it is a binary system, due to the regular variations and the presence of hard x-ray radiation

28″ along a position angle of 190°. The primary may itself be a close binary system with a separation of 0.3692″ and a magnitude difference of 3.97 at an

star with overall apparent visual magnitude +2.06, it is actually a binary system composed of two stars in close orbit. The chemical composition of the

their outer envelopes are in direct contact, making them a contact binary system. As a result, they have the same stellar classification of F8Vp, which

disk. All RV Tauri stars with dust disks are believed to be part of a binary system. Slow periodic variations in the mean brightness of SX Centauri have

forms a well-known naked eye double star with the fainter star Alcor (a binary system consisting of Alcor A and Alcor B), and is itself a quadruple star system

designated: 2003 QQ47, is a kilometer-sized asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid

provisional designation 1998 QE2, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid

41 Tauri is a single-lined spectroscopic binary system in the zodiacal constellation of Taurus; 41 Tauri is its Flamsteed designation. The star has a

light-years from Earth. In 2017, more accurate analysis found it to be a binary system made up of two substellar objects of spectral class≥Y1 in orbit less

provisional designation 1938 YG, is a rare-type Hungaria asteroid and binary system from the inner regions of the asteroid belt, approximately 8 kilometers

survey using Gaia DR2 data found WASP-64 to be the secondary star in a binary system, with a wide separation of 24.2 arcseconds or 9,058 AU. The primary

Cygni is about a degree away to the north, also a detached eclipsing binary system. It comprises a large cool evolved star and a small hot main sequence

upon variations in its proper motion, this is a probable astrometric binary system. As such, its two components would be designated Beta2 Sagittarii A

velocity of around 14 km/s, and it is suspected the rotations of this binary system may be synchronized. The system is a source for X-ray emission, which

giant of apparent magnitude 2.4. Next is Beta Phoenicis, actually a binary system composed of two yellow giants with a combined apparent magnitude of

However, recent evidence indicates that the star may actually be a binary system itself, consisting of two brown dwarfs, AB Doradus Ca/Cb, with 72 and

complex within the constellation Cygnus X-1, a binary system within the constellation Cygnus X-3, a binary system within the constellation Cygnus 20, a Canadian

maximum brightness. RT Aurigae has been suspected to be a spectroscopic binary system, but this has not been confirmed. The strongest evidence was found in

located about 310 light years away from the Sun. The components of this binary system have a separation of 7 AU, and are orbiting their common barycenter

telescope. Mizar and its fainter companion Alcor are actually a four-star binary system consisting of two pairs of double stars that are gravitationally bound

orbital plane is inclined near the line of sight, two form an eclipsing binary system. The eclipse of the primary component causes a 0.04 drop in magnitude

located 100 light years from the Sun. The pair form a close spectroscopic binary system with a physical separation of about 14.9 astronomical units. The primary

based on parallax measurements. There is some indication this may be a binary system, but the evidence is inconclusive. The variability of this star was

motion measurements. It is an unresolved, single-lined spectroscopic binary system with an orbital period of 1.39 years and an eccentricity (ovalness)

mass of the Earth. It is aligned to within 10° of the plane of the binary system. Henry, Gregory W.; Fekel, Francis C.; Hall, Douglas S. (December 1995)

occulted by the moon or planets. This is a single-lined spectroscopic binary system with an orbital period of 137.3 days and an eccentricity of 0.7. The

radial velocity variations that can be best explained as a spectroscopic binary system. The visible component is an A-type main-sequence star with a stellar

class of M5 and is overluminous for its type, which may mean it is a binary system. List of stars in Leo van Leeuwen, F. (2007), "Validation of the new

generally, tick–tock is an engineering model which refreshes one half of a binary system each release cycle. Every "tick" represented a shrinking of the process

Earth. Stein 2051 is the nearest (red dwarf + white dwarf) separate binary system (40 Eridani BC is located closer at 16.26 light-years, but it is a part

For example, stable trinary systems consist of two stars in a close binary system, with a third orbiting this pair at a distance much larger than that

located 100 light years from the Sun. The pair form a close spectroscopic binary system with a physical separation of about 14.9 astronomical units. The primary

about 192 light-years (59 parsecs) from Earth. This is a spectroscopic binary system, consisting of an orbiting pair of stars that have not been individually

RZ Pyxidis is eclipsing binary system in the constellation Pyxis, made up of two young stars less than two millions years old. Both are hot blue-white

first observed by H. A. Abt in 1961. It is a double-lined spectroscopic binary system with an orbital period of 27.2 days and an eccentricity of 0.74. They

variable star designation BZ Crucis. It is not known to be a member of a binary system, although it is probably a member of the open cluster NGC 4609. This

generalisation of Kepler's Third Law, which states that the total mass of a binary system multiplied by the square of its orbital period is proportional to the

Gamma Coronae Borealis, Latinized from γ Coronae Borealis, is a binary star system in the northern constellation of Corona Borealis. It is visible to the

UY Volantis, also known as EXO 0748-676, is a low mass X-ray binary system located in the constellation Volans. With an apparent magnitude of 16.9, it

association of co-moving stars. This is a double-lined spectroscopic binary system consisting of two F-type main-sequence stars with similar masses and

The spectrum also shows emission lines of HeII and OIV. WR 137 is a binary system, with an O9 main sequence or giant companion. The two stars orbit every

and smaller than the Sun). The other secondary stars are themselves a binary system, two red dwarfs that orbit the primary star. A brown dwarf has been

a stellar mass black hole with a mass between 3 and 10 M☉. It is a binary system in which a star orbits the black hole. Its small size may make it a

to the Sun with a radial velocity of −5 km/s. This is an astrometric binary system with a period of 6.5 years (2,374 days) and an orbital eccentricity

Sun with a heliocentric radial velocity of 6.4 km/s. This is a close binary system with an orbital period of 2.6 days and an orbital plane that is oriented

the components," whereas Eggleton and Tokovinin (2008) list it as a binary system. Gaia Data Release 2 gives a parallax of 1.0868±0.0391 mas for the companion

(450894) 2008 BT18 is a sub-kilometer asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the

designation 1924 QG, is a stony Florian asteroid and suspected asynchronous binary system from the inner regions of the asteroid belt, approximately 10 kilometers

primary member, designated component A, is a single-lined spectroscopic binary system in a circular orbit with a period of 3.7887 days. The visible member

in the light curve of V407 Lupi indicating an orbital period for the binary system of 3.513 days; it was previously thought to be 3.573 hours, but this

BP Crucis (x-ray source GX 301-2) is an X-ray binary system containing a blue hypergiant and a pulsar. BP Crucis is considered as the optical counterpart

although, as of 2015, there remains doubt as to whether this is an actual binary system. Kiss, Laszlo L. (July 1998). "A photometric and spectroscopic study

HD 134439 and HD 134440 are a pair of K-type runaway stars, nearly hypervelocity stars, in the constellation Libra. Although they are roughly 96 ly away

Noah's Ark).[citation needed] This is a single-lined spectroscopic binary system with an orbital period of 868.78 days and an eccentricity of 0.7. It

stellar classification of Upsilon Sagittarii difficult. υ Sgr is a binary system with an orbital period of 137.939 days and is approximately 1,800 light

of 0.27. This is a RS Canum Venaticorum variable, indicating a close binary system with active star spots, and has the variable star designation BC Psc

dwarf with an orbital period of 50.2 years. This is a shallow contact binary system, belonging to sub-type A of the W Ursae Majoris class. It has an orbital

and sampler; violinist; percussionist; and a shawm/sackbutt player. Binary System, an instrumental, piano/drums duo with percussionist Larry Dersch.

pair of stars separated by 41″, each of which is also a spectroscopic binary system. γ2 Velorum, the brighter of the visible pair, contains the Wolf–Rayet

223 light years from the Sun. This is a double-lined spectroscopic binary system with an orbital period of 40.58 days. The two components are nearly

with a heliocentric radial velocity of +1.47 km/s. Component A forms a binary system with an orbital period of 25.33 years, an eccentricity of 0.40, and

with the IUE spacecraft in 1985 showed that the companion is a close binary system with a period of 4.7 days. The members of this pair have classes of

abundances similar to an Am star. This is a double-lined spectroscopic binary system with an orbital period of 6.36246 days and an eccentricity (ovalness)

point for the annual Perseid meteor shower. This is a wide eclipsing binary system with an orbital period of 5,329.8 days (14.6 years). This eclipse was

announced in 1922 by W. W. Campbell. It is a single-lined spectroscopic binary system with an orbital period of 6.86 years and an eccentricity of 0.38. The

a radial velocity of +26 km/s. This is a single-lined spectroscopic binary system with an orbital period of 4.6 years and an eccentricity of around 0

candidates have been identified, formed from the merger of two stars in a binary system, and these are preferentially concentrated near the core region. It

by 0.054 in magnitude with no clear period. This is a spectroscopic binary system with an orbital period of 176 days. The companion is a subdwarf O star

This system is often confused with HD 216655, a slightly brighter binary system. HD 216655 is located 93.9" away from Tau2 Gruis and they appear to

Sun-like abundances of most elements. This is a probable astrometric binary system with poorly constrained orbital elements. The visible member, component

Japanese description of κ Geminorum. This is a probable astrometric binary system with the components having an angular separation of 7.2 arcseconds along

calculated from observable quantities only, namely the orbital period of the binary system, and the peak radial velocity of the observed star. The velocity of

the star's proper motion over time indicate this is an astrometric binary system. The visible component is an evolved G-type giant star with a stellar

interstellar dust. The inner pair form a double-lined spectroscopic binary system with an orbital period of 3.26 days and an eccentricity of 0.13. Both

variability with a period of 3.02 days. This suggests it is a close binary system forming a rotating ellipsoidal variable, although other causes such

mythology. In October 2018, it was reported that Antenor is likely a binary system. If confirmed, it would be 5th known binary Jupiter trojan. Antenor

hue of a B7 star main sequence star. The two stars form an eclipsing binary system (variable star designation: V1488 Cyg) similar to Algol. The orbital

an eccentricity of 0.39. The pair form a Beta Lyrae-type eclipsing binary system, dropping by magnitude 0.04 during the primary eclipse. This system

Oddly, the disk appears to be misaligned with the orbital plane of the binary system. This may be the result of an interaction within another star system

630 group of co-moving stars. This is a single-lined spectroscopic binary system with an orbital period of just 1.71 days in a circular orbit. The unresolved

a hot Jupiter found orbiting a star in a still visually unresolved binary system, was announced in June 2018. The data regarding the exoplanet is based

Chini et al. (2012) identified this as a single-lined spectroscopic binary system. The visible component is a B-type main-sequence star with a stellar

The Bibi-binary system for numeric notation (French: système Bibi-binaire, or abbreviated "système Bibi") is a hexadecimal numeral system first described

provisional designation 1934 XA, is a stony Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 7.8 kilometers

density of the primary was calculated using the orbital elements of the binary system, the primary-to-secondary mass ratio, and estimates of the primary size

designation 1994 KA, is a stony Phocaea asteroid and an asynchronous binary system from the inner regions of the asteroid belt, approximately 10 kilometers

variable star designation, V846 Arae, in 1999. This is a spectroscopic binary system, which means that the presence of an orbiting companion is indicated

provisional designation 1971 ME, is a stony Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 10 kilometers

discovered by W. Strohmeier, R. Knigge, and H. Ott in 1965. It is a detached binary system with both components filling three-fourths of their respective Roche

(provisional designation 2007 UK126) is a trans-Neptunian object and binary system from the extended scattered disc, located in the outermost region of

a radial velocity of −33 km/s. This is a double-lined spectroscopic binary system consisting of two near-identical, massive, O-type main sequence stars

Miller had previously played piano with percussionist Larry Dersch as Binary System but with the addition of bassist Andrew Willis, Miller switched back

light-years (13.48 parsecs). In 1976, this was reported as a spectroscopic binary system by Helmut A. Abt and Saul G. Levy, giving it an orbital period of 371

his system thus: I am not afraid, or do not hesitate, to advocate a binary system of arithmetic and metrology. I know I have nature on my side; if I do

as a single star, according to Kunzli and North (1998) it may be a binary system with a long orbital period. The visible component has a stellar classification

A Bancroft point is the temperature where an azeotrope occurs in a binary system. Although vapor liquid azeotropy is impossible for binary systems which

400 light years from the Sun. This is a suspected close spectroscopic binary system. The spectrum varies with a periodicity of 28.9 days, and a helium emission

Chaoyichi (provisional designation 1998 FL116) is a background asteroid and binary system from the inner region of the asteroid belt, approximately 2 kilometers

provisional designation 1984 JP1, is a Florian asteroid and a suspected binary system from the inner regions of the asteroid belt, approximately 6.9 kilometers

radial velocity of +18.7 km/s. This is a double-lined spectroscopic binary system with an orbital period of 260 days and an eccentricity of 0.005. The

designation 1971 UA1, is a bright Hungaria asteroid and synchronous binary system from the innermost regions of the asteroid belt, approximately 3.5 kilometers

binaries, H. Shapley listed a low orbital eccentricity of 0.091 for this binary system. He considered both eclipses to be partial, but only after correcting

variability with a period of about 1100 seconds. KIC 9246715 is an eclipsing binary system consisting of two red giants. The primary component of the system has

In astrophysics, the chirp mass of a compact binary system determines the leading-order orbital evolution of the system as a result of energy loss from

of 0.07 magnitude. Confirmation would indicate that this is a close binary system. It has an estimated age of around 57 million years. In Chinese, 子 (Zǐ)

0.2 magnitudes. The accepted model for this class of variable is a binary system with a red dwarf secondary in a close orbit with a magnetic white dwarf

variable star designation, Z Canis Majoris, in 1922. The star is a complex binary system only 300,000 years old with two main components separated by an estimated

along a position angle of 220°, as of 2010. The pair may form a wide binary system. van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction"

Shafter and F. V. Hessman in 1984 found this to be a close eclipsing binary system with a period of 3.27 hours. This is a nova-like binary where mass is

credit. By the laws of physics, it is easy to determine the mass of a binary system based on its orbital period, so Harrington was the first to calculate

luminosity of 11.5×1028 erg s−1. Eta Ursae Minoris may form a wide binary system with a magnitude 15.3 companion star, located at an angular separation

2623 Zech, provisional designation A919 SA, is a stony binary asteroid from the inner regions of the asteroid belt, approximately 6.5 kilometers in diameter

provisionally known as 1979 SW11, is a stony Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 4.7 kilometers

1998 WW31, is a non-resonant trans-Neptunian object and binary system from the Kuiper belt located in the outermost region of the Solar System, approximately

is a physically unrelated background star. HD 106515 AB is a wide binary system which was first observed by Jérôme de Lalande in 1795. The discovery

one that uses ternary logic (i.e., base 3) instead of the more common binary system (i.e., base 2) in its calculations. Ternary computers use trits, instead

credit. By the laws of physics, it is easy to determine the mass of a binary system based on its orbital period, so Harrington was the first to calculate

1998 WW31, is a non-resonant trans-Neptunian object and binary system from the Kuiper belt located in the outermost region of the Solar System, approximately

V691 Coronae Australis (abbreviated V691 CrA), is a neutron-star X-ray binary system at a distance of approximately 2-2.5 kiloparsecs. It is known to have

member of the Tucana–Horologium stellar kinematic group. This is a wide binary system with a projected separation of 184.3 AU. Two sets of low quality orbital

binary system whose combined mass is estimated, per 2008 calculations, to be almost 100 solar masses. Monoceros is the location of the binary system Scholz's

1866 Sisyphus /ˈsɪsɪfəs/ is a binary stony asteroid, near-Earth object and the largest member of the Apollo group, approximately 7 kilometers in diameter

R Coronae Australis (R CrA) is a variable binary system in the constellation Corona Australis. It has varied between magnitudes 10 and 14.36. A small

was determined to be a short period, strongly-interacting eclipsing binary system. Observations of the light variations up until 1979 were used by G.

Ab is an exoplanet that orbits WASP-85 A, a star that is part of a binary system. WASP-85 Ab's mass and radius indicate that it has a bulk composition

provisional designation 1994 LE3, is a Hungaria asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 3 kilometers

in 2006/7, it was revealed that Iwamoto ("primary") is a synchronous binary system with a minor-planet moon ("secondary") orbiting it every 4.917 days

127 light-years distant from Earth. It is actually a spectroscopic binary system; the primary is a white star of spectral type A5IV with 3.5 times the

younger, has high metallicity, has much cooler temperature and is in a binary system. As of 2000, it has been confirmed that an extrasolar planet orbits

provisional designation 1933 QG, is a background asteroid and synchronous binary system from the Eunomian region in the central asteroid belt, approximately

estimate of its distance as 81 light years. This is a candidate wide binary system as a faint companion star shares a common proper motion with the brighter

3 over a period of 3.298 days, although it is actually an eclipsing binary system rather than a pulsating star. AX is a Cepheid variable that varies between

English: the Seventh Star of Celestial Dog.) This is an astrometric binary system, as determined by changes in the proper motion of the primary. The visible

Crateris is located 87 light years from the Sun. This is an astrometric binary system with an estimated orbital period of roughly 79,000 years. The primary

2001 QW322 is a trans-Neptunian object and binary system of the Kuiper belt, located in the outermost region of the Solar System. The cubewano was discovered

3905 Doppler, provisional designation 1984 QO, is a stony asteroid and binary system from the middle region of the asteroid belt, approximately 8 kilometers

provisional designation 1989 UN2, is a bright Hungaria asteroid and suspected binary system from the innermost regions of the asteroid belt, approximately 2 kilometers

designation 1989 AA5, is a stony background asteroid and asynchronous binary system from the inner regions of the asteroid belt, approximately 8 kilometers

2754 Efimov, provisionally named 1966 PD, is a stony asteroid and binary system from the inner regions of the asteroid belt, approximately 5 kilometers

−37 km/s. Griffin (2012) found this to be a single-lined spectroscopic binary system with an orbital period of 2.7373 ± 0.0066 yr and an eccentricity of

(410777) 2009 FD is a carbonaceous sub-kilometer asteroid and binary system, classified as near-Earth object and potentially hazardous asteroid of the

Carina–Sagittarius Arm, and is a member of an occulting spectroscopic binary system. The visible component is Krzemiński's Star, a supergiant; the X-ray

main-sequence companion separated by 34.8″. Together, they make up a wide binary system designated collectively as CPD−76°1542. Sir John Herschel, the discoverer

(/ɪfˈθaɪmiː/; provisional designation 1998 WR21) is a Jupiter trojan and a binary system from the Greek camp, approximately 57 kilometers (35 miles) in diameter

(prov. designation: 1986 JN1) is a bright Hungaria asteroid, suspected binary system and asteroid pair from the innermost regions of the asteroid belt, approximately

provisionally designated 1981 JC, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 10 kilometers

velocity by J. H. Moore in 1910. It is a single-lined spectroscopic binary system with an orbital period of 2.05 years and an eccentricity (ovalness)

used to accurately identify these optical counterparts. X Persei is a binary system containing a γ Cassiopeiae variable and a pulsar. It has a relatively

(26308) 1998 SM165 is a resonant trans-Neptunian object and binary system from the Kuiper belt in the outermost regions of the Solar System. It was discovered

two revolve around each other every 2.24 years. Farther afield is a binary system of two G-type main sequence stars, that would take 170,000 years to

provisional designation 1986 CK1, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 7 kilometers

dwarf, which gets depleted of hydrogen via mass transfer in a close binary system with a second, massive object like a neutron star. One scenario involves

Sérsic, provisional designation 1974 KB, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 6 kilometers

provisional designation 1997 QN1, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 3.5 kilometers

(Lěi Bì Zhèn èr, English: the Second Star of Line of Ramparts.) The binary system has an orbital period of 129 days. The primary, component Aa, is a Be

magnitude stars and many fainter stars. S Monocerotis A is a spectroscopic binary system with an eccentric orbit of about 112 years. Since 1943, the spectrum

this star is approximately 260 light years. The inner pair is a visual binary system consisting of two A-type main-sequence stars with an orbital period

Sérsic, provisional designation 1974 KB, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 6 kilometers

population belongs to the 80 largest Jupiter trojans. It is a suspected binary system and potentially a slow rotator with a rotation period of 479 hours.

(175706) 1996 FG3 is a carbonaceous asteroid and binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group

provisional designation 1939 FY, is a stony asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 10 kilometers

around −6 km/s. Iota Trianguli Australis is a double-lined spectroscopic binary system with an orbital period of 39.88 days and an eccentricity of 0.25. The

astrophysics. In 1974, Hulse and Taylor discovered the first pulsar in a binary system, named PSR B1913+16 after its position in the sky, during a survey for

presumably formed by the merger of two stars or by interactions in a binary system. This explains why SX Phoenicis seems to be a young star, despite belonging

primary, designated component A, is itself a double-lined spectroscopic binary system with an orbital period of 2.26 days and an eccentricity of 0.08. The

the main sequence. 2 Lacertae is a rotating ellipsoidal variable, a binary system in which the stars are close enough to each other for one or both stars

(31345) 1998 PG is an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters

provisional designation 1983 VG7, is a stony Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 5 kilometers

designation 1988 BO2, is a stony Phocean asteroid and a potentially binary system from the inner regions of the asteroid belt, approximately 9 kilometers

provisional designation 1989 CJ1, is a Hungaria asteroid and synchronous binary system from the innermost regions of the asteroid belt, approximately 4 kilometers

Mathys and associates (1997) demonstrated this is a spectroscopic binary system. This single-lined spectroscopic binary has a physical separation of

1717 Arlon, provisional designation 1954 AC, is a binary Florian asteroid from the inner regions of the asteroid belt, approximately 8.5 kilometers in

(provisional designation 1979 UC4) is a stony background asteroid and binary system from the middle regions of the asteroid belt, approximately 3 kilometers

Binzel, provisional designation 1982 FR, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 6.5 kilometers

/əˈlɔːdə/, provisional designation 1910 KQ, is a carbonaceous asteroid and binary system from the outer asteroid belt, approximately 190 kilometers in diameter

of stars that share a common motion through space. It forms a wide binary system with the star HD 181327 and has a substellar companion orbiting around

1984 WB, is a stony Hungarian asteroid, Mars-crosser and suspected binary system, from the innermost regions of the asteroid belt, approximately 7 kilometers

located about 1,055 parsecs (3,440 light-years) away from Earth. The binary system is composed of a G-type main sequence star (Kepler-47A) and a red dwarf

designation 1927 WB, is an elongated Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 12 kilometers

scenarios require either the evolution of a triple star system, or a binary system with highly eccentric orbit resulting in grazing interactions. The dwarf

The system is drifting closer with a radial velocity of −21 km/s. The binary system consists of a bright giant orbited by a dwarf companion once every four

is a stony Hungaria asteroid, Mars-crosser and suspected synchronous binary system from the innermost regions of the asteroid belt, approximately 4 kilometers

receding with a radial velocity of 34 km/s. This is a spectroscopic binary system with an orbital period of 2.97 days and an eccentricity of 0.10. The

Jorge; Ramírez, Iván (2014). "High Precision Abundances in the 16 Cyg Binary System: A Signature of the Rocky Core in the Giant Planet". The Astrophysical

designation: 1988 SH) is a dark and elongated background asteroid and binary system from the intermediate asteroid belt, approximately 15 kilometers (9

(provisional designation 2000 HM53) is a background asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 4 kilometers

eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude

eclipse and 4.83 in the secondary eclipse. It is probably a detached binary system with no circumstellar material being found. Both components of this

the detection of a third body of planetary mass around the eclipsing binary system. The presence of a third body had already been suspected in 2002. The

White dwarfs are the remnants of low-mass stars which, if they form a binary system with another star, can cause large stellar explosions known as type

Mendoza, provisional designation 4575 P-L is a stony Vestian asteroid and binary system from the inner regions of the asteroid belt, approximately 9 kilometers

Zwicky, prov. designation: 1967 CA, is a stony Phocaea asteroid and binary system from the inner regions of the asteroid belt, approximately 10 kilometers

Bridges, provisional designation 1982 KC1, is a stony asteroid and binary system from the middle regions of the asteroid belt, approximately 8 kilometers

Taurus Molecular Cloud. The stars GK Tauri and GI Tauri form a wide binary system, with the projected separation between components being 1700 AU. The

binary system derives a distance of 1,310±60 pc. On this basis, it is thought to be a member of the NGC 6530 open cluster. 9 Sagittarii is a binary system

observed in the Quintuplet Cluster. The archetype of such a colliding-wind binary system is WR 140 (HD 193793), which consists of a 20 solar mass (M☉) Wolf-Rayet

An intermediate-mass binary pulsar (IMBP) is a pulsar-white dwarf binary system with a relatively long spin period of around 10–200 ms consisting of

(provisional designation 1991 CU2) is a stony Nysian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 5 kilometers

designation 1975 AN, is a stony Phocaean asteroid, sizable Mars-crosser, and binary system on an eccentric orbit from the inner regions of the asteroid belt, approximately

1798 Watts, provisional designation 1949 GC, is a stony asteroid and binary system from the inner regions of the asteroid belt, approximately 7 kilometers

at the Palomar Observatory in California. The unlikely synchronous binary system has a rotation period of 3.3 hours. It was named after the discoverer's

provisional designation 1988 XE1, is a Vestian asteroid and suspected binary system from the inner regions of the asteroid belt, approximately 6 kilometers

Meintjes, P. J.; Yadav, K. K. (2021). "Properties of white dwarf in the binary system AR Scorpii and its observed features". Modern Physics Letters A. 36