Vega

Vega

Location of Vega in the constellation Lyra
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Lyra
Pronunciation	/ˈviːɡə/ or /ˈveɪɡə/
Right ascension	18h 36m 56.33635s[1]
Declination	+38° 47′ 01.2802″[1]
Apparent magnitude (V)	0.03[2]
Characteristics
Spectral type	A0V[3]
U−B color index	−0.01[2]
B−V color index	+0.00[2]
Variable type	Suspected Delta Scuti[4]
Astrometry
Radial velocity (Rv)	−13.9 ± 0.9[5] km/s
Proper motion (μ)	RA: 200.94[1] mas/yr Dec.: 286.23[1] mas/yr
Parallax (π)	130.23 ± 0.36[1] mas
Distance	25.04 ± 0.07 ly (7.68 ± 0.02 pc)
Absolute magnitude (MV)	0.58[note 1]
Details
Mass	2.135 ± 0.074[6] M☉
Radius	2.362 × 2.818[6] R☉
Luminosity	40.12 ± 0.45[6] L☉
Surface gravity (log g)	4.1 & 0.1[7] cgs
Temperature	9,602 ± 180[8] (8,152–10,060 K)[6] K
Metallicity [Fe/H]	−0.5[8] dex
Rotation	12.5 h
Rotational velocity (v sin i)	20.48 ± 0.11[6] km/s
Age	455 ± 13[6] Myr
Other designations
Wega,[9] Lucida Lyrae,[10] Alpha Lyrae, α Lyrae, 3 Lyr, GJ 721, HR 7001, BD +38°3238, HD 172167, GCTP 4293.00, LTT 15486, SAO 67174, HIP 91262,[2] 织女一

Vega (α Lyr, α Lyrae, Alpha Lyrae) is the brightest star in the constellation Lyra, the fifth brightest star in the night sky and the second brightest star in the northern celestial hemisphere, after Arcturus. It is a relatively close star at only 25 light-years from Earth, and, together with Arcturus and Sirius, one of the most luminous stars in the Sun's neighborhood.

Vega has been extensively studied by astronomers, leading it to be termed "arguably the next most important star in the sky after the Sun."^[11] Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727 when the declination will be +86°14'.^[12] Vega was the first star other than the Sun to be photographed and the first to have its spectrum recorded. It was one of the first stars whose distance was estimated through parallax measurements. Vega has served as the baseline for calibrating the photometric brightness scale, and was one of the stars used to define the mean values for the UBV photometric system.

Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their life expectancies. Vega has an unusually low abundance of the elements with a higher atomic number than that of helium.^[8] Vega is also a suspected variable star that may vary slightly in magnitude in a periodic manner.^[13] It is rotating rapidly with a velocity of 274 km/s at the equator. This is causing the equator to bulge outward because of centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is being observed from the direction of one of these poles.^[14]

Based on an observed excess emission of infrared radiation, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System.^[15] Stars that display an infrared excess because of dust emission are termed Vega-like stars.^[16] Irregularities in Vega's disk also suggest the presence of at least one planet, likely to be about the size of Jupiter,^[17] in orbit around Vega.^[18]

Observation history

Astrophotography, the photography of celestial objects, began in 1840 when John William Draper took an image of the Moon using the daguerreotype process. On July 17, 1850, Vega became the first star (other than the Sun) to be photographed, when it was imaged by William Bond and John Adams Whipple at the Harvard College Observatory, also with a daguerreotype.^[9][19][20] Henry Draper took the first photograph of a star's spectrum in August 1872 when he took an image of Vega, and he also became the first person to show absorption lines in the spectrum of a star.^[21] Similar lines had already been identified in the spectrum of the Sun.^[22] In 1879, William Huggins used photographs of the spectra of Vega and similar stars to identify a set of twelve "very strong lines" that were common to this stellar category. These were later identified as lines from the Hydrogen Balmer series.^[23] Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.^[24]

The distance to Vega can be determined by measuring its parallax shift against the background stars as the Earth orbits the Sun. The first person to publish a star's parallax was Friedrich G. W. von Struve, when he announced a value of 0.125 arcseconds (0.125″) for Vega.^[25] But Friedrich Bessel was skeptical about Struve's data, and, when Bessel published a parallax of 0.314″ for the star system 61 Cygni, Struve revised his value for Vega's parallax to nearly double the original estimate. This change cast further doubt on Struve's data. Thus most astronomers at the time, including Struve, credited Bessel with the first published parallax result. However, Struve's initial result was actually surprisingly close to the currently accepted value of 0.129″,^[26][27] as determined by the Hipparcos astrometry satellite.^[1][28][29]

The brightness of a star, as seen from Earth, is measured with a standardized, logarithmic scale. This apparent magnitude is a numerical value that decreases in value with increasing brightness of the star. The faintest stars visible to the unaided eye are sixth magnitude, while the brightest, Sirius, is of magnitude −1.46. To standardize the magnitude scale, astronomers chose Vega to represent magnitude zero at all wavelengths. Thus, for many years, Vega was used as a baseline for the calibration of absolute photometric brightness scales.^[30] However, this is no longer the case, as the apparent magnitude zero point is now commonly defined in terms of a particular numerically specified flux. This approach is more convenient for astronomers, since Vega is not always available for calibration.^[31]

The UBV photometric system measures the magnitude of stars through ultraviolet, blue, and yellow filters, producing U, B, and V values, respectively. Vega is one of six A0V stars that were used to set the initial mean values for this photometric system when it was introduced in the 1950s. The mean magnitudes for these six stars were defined as: U − B = B − V = 0. In effect, the magnitude scale has been calibrated so that the magnitude of these stars is the same in the yellow, blue, and ultraviolet parts of the electromagnetic spectrum.^[32] Thus, Vega has a relatively flat electromagnetic spectrum in the visual region—wavelength range 350–850 nanometers, most of which can be seen with the human eye—so the flux densities are roughly equal; 2000–4000 Jy.^[33] However, the flux density of Vega drops rapidly in the infrared, and is near 100 Jy at 5 micrometers.^[34]

Photometric measurements of Vega during the 1930s appeared to show that the star had a low-magnitude variability on the order of ±0.03 magnitudes. This range of variability was near the limits of observational capability for that time, and so the subject of Vega's variability has been controversial. The magnitude of Vega was measured again in 1981 at the David Dunlap Observatory and showed some slight variability. Thus it was suggested that Vega showed occasional low-amplitude pulsations associated with a Delta Scuti variable.^[4] This is a category of stars that oscillate in a coherent manner, resulting in periodic pulsations in the star's luminosity.^[35] Although Vega fits the physical profile for this type of variable, other observers have found no such variation. Thus the variability was thought to possibly be the result of systematic errors in measurement.^[13][36] However, a 2007 article surveyed these and other results, and concluded that "A conservative analysis of the foregoing results suggests that Vega is quite likely variable in the 1-2% range, with possible occasional excursions to as much as 4% from the mean.".^[37] Also, a 2011 article affirms on its abstract that "The long-term (year-to-year) variability of Vega was confirmed".^[38]

Vega became the first solitary main-sequence star beyond the Sun known to be an X-ray emitter when in 1979 it was observed from an imaging X-ray telescope launched on an Aerobee 350 from the White Sands Missile Range.^[39] In 1983, Vega became the first star found to have a disk of dust. The Infrared Astronomical Satellite (IRAS) discovered an excess of infrared radiation coming from the star, and this was attributed to energy emitted by the orbiting dust as it was heated by the star.^[40]

Visibility

Vega can often be seen near the zenith in the mid-northern latitudes during the evening in the Northern Hemisphere summer.^[41] From mid-southern latitudes, it can be seen low above the northern horizon during the Southern Hemisphere winter. With a declination of +38.78°, Vega can only be viewed at latitudes north of 51° S. Therefore, it does not rise at all anywhere in Antarctica or in the southernmost part of South America, including Punta Arenas, Chile (53° S). At latitudes to the north of +51° N, Vega remains continually above the horizon as a circumpolar star. Around July 1, Vega reaches midnight culmination when it crosses the meridian at that time.^[42]

This star lies at a vertex of a widely spaced asterism called the Summer Triangle, which consists of the zero-magnitude stars Vega in the constellation Lyra and Altair in Aquila, plus the first magnitude star Deneb in Cygnus.^[41] This formation is the approximate shape of a right triangle, with Vega located at its right angle. The Summer Triangle is recognizable in the northern skies for there are few other bright stars in its vicinity.^[43] Vega can be identified easily because Altair and its two neighbouring stars form a line which points at Vega.

The Lyrids is a strong meteor shower that peaks each year during April 21–22. When a small meteor enters the Earth's atmosphere at a high velocity, it produces a streak of light as the object is vaporized. During a shower, a multitude of meteors arrive from the same direction, and, from the perspective of an observer, their glowing trails appear to radiate from a single point in space. In the case of the Lyrids, the meteor trails radiate from the direction of Lyra, and hence are sometimes called the Alpha Lyrids. However, they actually originated from debris emitted by the comet C/1861 G1 Thatcher and have nothing to do with the star.^[44]

Physical properties

Vega's spectral class is A0V, making it a blue-tinged white main sequence star that is fusing hydrogen to helium in its core. Since more massive stars use their fusion fuel more quickly than smaller ones, Vega's main-sequence lifetime is roughly one billion years, a tenth of our Sun's.^[45] The current age of this star is about 455 million years,^[6] or up to about half its expected total main-sequence lifespan. After leaving the main sequence, Vega will become a class-M red giant and shed much of its mass, finally becoming a white dwarf. At present, Vega has more than twice the mass^[14] of the Sun and its full luminosity is about 40 times the Sun's value. However, because of its high rate of rotation, the pole is considerably brighter than the equator. Since we see it nearly pole-on, its apparent luminosity from Earth is notably higher, about 57 times the Sun's value.^[7] If Vega is variable, then it may be a Delta Scuti type with a period of about 0.107 days.^[4]

Most of the energy produced at Vega's core is generated by the carbon–nitrogen–oxygen cycle (CNO cycle), a nuclear fusion process that combines protons to form helium nuclei through intermediary nuclei of carbon, nitrogen, and oxygen. This process requires a temperature of about 15 million K,^[46] which is higher than the core temperature of the Sun, but is less efficient than the Sun's proton-proton chain reaction fusion reaction. The CNO cycle is highly temperature sensitive, which results in a convection zone about the core^[47] that evenly distributes the 'ash' from the fusion reaction within the core region. The overlying atmosphere is in radiative equilibrium. This is in contrast to the Sun, which has a radiation zone centered on the core with an overlying convection zone.^[48][49]

The energy flux from Vega has been precisely measured against standard light sources. At 5480 Å, the flux is 3,650 Jy with an error margin of 2%.^[50] The visual spectrum of Vega is dominated by absorption lines of hydrogen; specifically by the hydrogen Balmer series with the electron at the n=2 principal quantum number.^[51][52] The lines of other elements are relatively weak, with the strongest being ionized magnesium, iron, and chromium.^[53] The X-ray emission from Vega is very low, demonstrating that the corona for this star must be very weak or non-existent.^[54] However, as the pole of Vega is facing us and a polar coronal hole may be present,^[39][55] confirmation of a corona as the likely source of the X-rays detected from Vega (or the region very close to Vega) may be difficult as most of any coronal X-rays would not be emitted along the line of sight.^[55][56]

Using spectropolarimetry, a magnetic field has been detected on the surface of Vega by a team of astronomers at the Observatoire du Pic du Midi. This is the first such detection of a magnetic field on a spectral class A star that is not an Ap chemically peculiar star. The average line of sight component of this field has a strength of −0.6 ± 0.3 G.^[57] This is comparable to the mean magnetic field on the Sun.^[58] Magnetic fields of roughly 30 gauss have been reported for Vega, compared to about 1 gauss for the Sun.^[39]

Rotation

When the radius of Vega was measured to high accuracy with an interferometer, it resulted in an unexpectedly large estimated value of 2.73 ± 0.01 times the radius of the Sun. This is 60% larger than the radius of the star Sirius, while stellar models indicated it should only be about 12% larger. However, this discrepancy can be explained if Vega is a rapidly rotating star that is being viewed from the direction of its pole of rotation. Observations by the CHARA array in 2005–06 confirmed this deduction.^[7]

The pole of Vega—its axis of rotation—is inclined no more than five degrees from the line-of-sight to the Earth. At the high end of estimates for the rotation velocity for Vega is 236.2 ± 3.7 km/s^[6] along the equator (for a rotation period of about 12.5 hours),^[14] which is 87.6% of the speed that would cause the star to start breaking up from centrifugal effects.^[6] This rapid rotation of Vega produces a pronounced equatorial bulge, so the radius of the equator is 19% larger than the polar radius. (The estimated polar radius of this star is 2.362 ± 0.012 solar radii, while the equatorial radius is 2.818 ± 0.013 solar radii.^[6]) From the Earth, this bulge is being viewed from the direction of its pole, producing the overly large radius estimate.

The local gravitational acceleration at the poles is greater than at the equator, so, by the Von Zeipel theorem, the local luminosity is also higher at the poles. This is seen as a variation in effective temperature over the star: the polar temperature is near 10,000 K, while the equatorial temperature is 7,600 K.^[14] As a result, if Vega were viewed along the plane of its equator, then the luminosity would be about half the apparent luminosity as viewed from the pole.^{[11][note 2]} This large temperature difference between the poles and the equator produces a strong 'gravity darkening' effect. As viewed from the poles, this results in a darker (lower intensity) limb than would normally be expected for a spherically symmetric star. The temperature gradient may also mean Vega has a convection zone around the equator,^[7][59] while the remainder of the atmosphere is likely to be in almost pure radiative equilibrium.^[60]

As Vega had long been used as a standard star for calibrating telescopes, the discovery that it is rapidly rotating may challenge some of the underlying assumptions that were based on it being spherically symmetric. With the viewing angle and rotation rate of Vega now better known, this will allow for improved instrument calibrations.^[61]

Element abundance

Astronomers term "metals" those elements with higher atomic numbers than helium. The metallicity of Vega's photosphere is only about 32% of the abundance of heavy elements in the Sun's atmosphere.^{[note 3]} (Compare this, for example, to a three-fold metallicity abundance in the similar star Sirius as compared to the Sun.) For comparison, the Sun has an abundance of elements heavier than helium of about Z_Sol = 0.0172 ± 0.002.^[62] Thus, in terms of abundances, only about 0.54% of Vega consists of elements heavier than helium.

The unusually low metallicity of Vega makes it a weak Lambda Boötis-type star.^[63][64] However, the reason for the existence of such chemically peculiar, spectral class A0-F0 stars remains unclear. One possibility is that the chemical peculiarity may be the result of diffusion or mass loss, although stellar models show that this would normally only occur near the end of a star's hydrogen-burning lifespan. Another possibility is that the star formed from an interstellar medium of gas and dust that was unusually metal-poor.^[65]

The observed helium to hydrogen ratio in Vega is 0.030 ± 0.005, which is about 40% lower than the Sun. This may be caused by the disappearance of a helium convection zone near the surface. Energy transfer is instead performed by the radiative process, which may be causing an abundance anomaly through diffusion.^[66]

Kinematics

The radial velocity of Vega is the component of this star's motion along the line-of-sight to the Earth. Movement away from the Earth will cause the light from Vega to shift to a lower frequency (toward the red), or to a higher frequency (toward the blue) if the motion is toward the Earth. Thus the velocity can be measured from the amount of redshift (or blueshift) of the star's spectrum. Precise measurements of this redshift give a value of −13.9 ± 0.9 km/s.^[5] The minus sign indicates a relative motion toward the Earth.

Motion transverse to the line of sight causes the position of Vega to shift with respect to the more distant background stars. Careful measurement of the star's position allows this angular movement, known as proper motion, to be calculated. Vega's proper motion is 202.03 ± 0.63 milli-arcseconds (mas) per year in right ascension—the celestial equivalent of longitude—and 287.47 ± 0.54 mas/y in declination, which is equivalent to a change in latitude. The net proper motion of Vega is 327.78 mas/y,^[67] which results in angular movement of a degree every 11,000 years.

In the Galactic coordinate system, the space velocity components of Vega are (U, V, W) = (−16.1 ± 0.3, −6.3 ± 0.8, −7.7 ± 0.3) km/s, for a net space velocity of 19 km/s.^[68] The radial component of this velocity—in the direction of the Sun—is −13.9 km/s, while the transverse velocity is 9.9 km/s. Although Vega is at present only the fifth-brightest star in the sky, the star is slowly brightening as proper motion causes it to approach the Sun.^[69] Vega will eventually become the brightest star in the sky in around 210,000 years, will attain a peak brightness of magnitude –0.81 in about 290,000 years and will be the brightest star in the sky for about 270,000 years.^[70]

Based on this star's kinematic properties, it appears to belong to a stellar association called the Castor Moving Group. However, Vega may be much older than this group, so the membership remains uncertain.^[6] This group contains about 16 stars, including Alpha Librae, Alpha Cephei, Castor, Fomalhaut and Vega. All members of the group are moving in nearly the same direction with similar space velocities. Membership in a moving group implies a common origin for these stars in an open cluster that has since become gravitationally unbound.^[71] The estimated age of this moving group is 200 ± 100 million years, and they have an average space velocity of 16.5 km/s.^{[note 4][68]}

Planetary system

Infrared excess

One of the early results from the Infrared Astronomy Satellite (IRAS) was the discovery of excess infrared flux coming from Vega, beyond what would be expected from the star alone. This excess was measured at wavelengths of 25, 60, and 100 μm, and came from within an angular radius of 10 arcseconds (10″) centered on the star. At the measured distance of Vega, this corresponded to an actual radius of 80 astronomical units (AU), where an AU is the average radius of the Earth's orbit around the Sun. It was proposed that this radiation came from a field of orbiting particles with a dimension on the order of a millimeter, as anything smaller would eventually be removed from the system by radiation pressure or drawn into the star by means of Poynting–Robertson drag.^[72] The latter is the result of radiation pressure creating an effective force that opposes the orbital motion of a dust particle, causing it to spiral inward. This effect is most pronounced for tiny particles that are closer to the star.^[73]

Subsequent measurements of Vega at 193 μm showed a lower than expected flux for the hypothesized particles, suggesting that they must instead be on the order of 100 μm or less. To maintain this amount of dust in orbit around Vega, a continual source of replenishment would be required. A proposed mechanism for maintaining the dust was a disk of coalesced bodies that were in the process of collapsing to form a planet.^[72] Models fitted to the dust distribution around Vega indicate that it is a 120 AU-radius circular disk viewed from nearly pole-on. In addition, there is a hole in the center of the disk with a radius of no less than 80 AU.^[74]

Following the discovery of an infrared excess around Vega, other stars have been found that display a similar anomaly that is attributable to dust emission. As of 2002, about 400 of these stars have been found, and they have come to be termed "Vega-like" or "Vega-excess" stars. It is believed that these may provide clues to the origin of the Solar System.^[16]

Debris disks

By 2005, the Spitzer Space Telescope had produced high-resolution infrared images of the dust around Vega. It was shown to extend out to 43″ (330 AU) at a wavelength of 24 μm, 70″ (543 AU) at 70 μm and 105″ (815 AU) at 160 μm. These much wider disks were found to be circular and free of clumps, with dust particles ranging from 1–50 μm in size. The estimated total mass of this dust is 3×10⁻³ times the mass of the Earth. Production of the dust would require collisions between asteroids in a population corresponding to the Kuiper Belt around the Sun. Thus the dust is more likely created by a debris disk around Vega, rather than from a protoplanetary disk as was earlier thought.^[15]

The inner boundary of the debris disk was estimated at 11″ ± 2″, or 70–100 AU. The disk of dust is produced as radiation pressure from Vega pushes debris from collisions of larger objects outward. However, continuous production of the amount of dust observed over the course of Vega's lifetime would require an enormous starting mass—estimated as hundreds of times the mass of Jupiter. Hence it is more likely to have been produced as the result of a relatively recent breakup of a moderate-sized (or larger) comet or asteroid, which then further fragmented as the result of collisions between the smaller components and other bodies. This dusty disk would be relatively young on the time scale of the star's age, and it will eventually be removed unless other collision events supply more dust.^[15]

Observations, first with the Palomar Testbed Interferometer in 2001^[75] and then later confirmed with the CHARA array at Mt. Wilson in 2006, revealed evidence for an inner dust band around Vega. Originating within 8 AU of the star, this exozodiacal dust may be evidence of dynamical perturbations within the system.^[76] This may be caused by an intense bombardment of comets or meteors, and may be evidence for the existence of a planetary system.^[77]

Possible planets

Observations from the James Clerk Maxwell Telescope in 1997 revealed an "elongated bright central region" that peaked at 9″ (70 AU) to the northeast of Vega. This was hypothesized as either a perturbation of the dust disk by a planet or else an orbiting object that was surrounded by dust. However, images by the Keck telescope had ruled out a companion down to magnitude 16, which would correspond to a body with more than 12 times the mass of Jupiter.^[78] Astronomers at the Joint Astronomy Centre in Hawaii and at UCLA suggested that the image may indicate a planetary system still undergoing formation.^[79]

Determining the nature of the planet has not been straightforward; a 2002 paper hypothesizes that the lumps are caused by a roughly Jupiter-mass planet on an eccentric orbit. Dust would collect in orbits that have mean-motion resonances with this planet—where their orbital periods form integer fractions with the period of the planet—producing the resulting clumpiness.^[17]

In 2003 it was hypothesized that these lumps could be caused by a roughly Neptune-mass planet having migrated from 40 to 65 AU over 56 million years,^[18] an orbit large enough to allow the formation of smaller rocky planets closer to Vega. The migration of this planet would likely require gravitational interaction with a second, higher-mass planet in a smaller orbit.^[80]

Using a coronagraph on the Subaru telescope in Hawaii in 2005, astronomers were able to further constrain the size of a planet orbiting Vega to no more than 5–10 times the mass of Jupiter.^[81] The issue of possible clumps in the debris disc was revisited in 2007 using newer, more sensitive instrumentation on the Plateau de Bure Interferometer. The observations showed that the debris ring is smooth and symmetric. No evidence was found of the blobs reported earlier, casting doubts on the hypothesized giant planet.^[82]

Although a planet has yet to be directly observed around Vega, the presence of a planetary system can not yet be precluded. Thus there could be smaller, terrestrial planets orbiting closer to the star. The inclination of planetary orbits around Vega is likely to be closely aligned to the equatorial plane of this star.^[83] From the perspective of an observer on a hypothetical planet around Vega, the Sun would appear as a faint 4.3 magnitude star in the Columba constellation.^{[note 5]}

Etymology and cultural significance

The name Wega^[9] (later Vega) comes from a loose transliteration of the Arabic word wāqi‘ meaning "falling" or "landing", via the phrase an-nasr al-wāqi‘, "the falling eagle".^[84] The term "Al Nesr al Waki" appeared in the Al Achsasi Al Mouakket star catalogue and was translated into Latin as Vultur Cadens, "the falling eagle/vulture".^{[85][note 6]} The constellation was represented as a vulture in ancient Egypt,^[86] and as an eagle or vulture in ancient India.^[87][88] The Arabic name then appeared in the western world in the Alfonsine Tables,^[89] which were drawn up between 1215 and 1270 by order of Alfonso X.^[90] Medieval astrolabes of England and Western Europe used the names Wega and Alvaca, and depicted it and Altair as birds.^[91]

Each night the positions of the stars appear to change as the Earth rotates. However, when a star is located along the Earth's axis of rotation, it will remain in the same position and thus is called a pole star. The direction of the Earth's axis of rotation gradually changes over time in a process known as the precession of the equinoxes. A complete precession cycle requires 25,770 years,^[92] during which time the pole of the Earth's rotation follows a circular path across the celestial sphere that passes near several prominent stars. At present the pole star is Polaris, but around 12,000 BC the pole was pointed only five degrees away from Vega. Through precession, the pole will again pass near Vega around AD 14,000.^[93] It is the brightest of the successive northern pole stars.^[9]

Among the northern Polynesian people, Vega was known as whetu o te tau, the year star. For a period of history it marked the start of their new year when the ground would be prepared for planting. Eventually this function became denoted by the Pleiades.^[94]

The Assyrians named this pole star Dayan-same, the "Judge of Heaven", while in Akkadian it was Tir-anna, "Life of Heaven". In Babylonian astronomy, Vega may have been one of the stars named Dilgan, "the Messenger of Light". To the ancient Greeks, the constellation Lyra was formed from the harp of Orpheus, with Vega as its handle.^[10] For the Roman Empire, the start of autumn was based upon the hour at which Vega set below the horizon.^[9]

In Chinese mythology, there is a love story of Qi Xi (七夕) in which Niu Lang (牛郎, Altair) and his two children (β and γ Aquilae) are separated from their mother Zhi Nü (織女, lit. "Weaving Girl", Vega) who is on the far side of the river, the Milky Way.^[95] However, one day per year on the seventh day of the seventh month of the Chinese lunisolar calendar, magpies make a bridge so that Niu Lang and Zhi Nü can be together again for a brief encounter. The Japanese Tanabata festival, in which Vega is known as orihime (織姫), is also based on this legend.^[96]

Vega is mentioned in a Chinese legend about Zhang Qian, though some argue that the historical person is not the subject of the legend; he just shared a name.^[97] It was said that he was commissioned to find the source of the Yellow River, which was believed to flow from heaven as a continuation of the Milky Way. After sailing up-river for many days, he saw a girl spinning and a cow herd. Upon asking the girl where he was, she presented him with her shuttle with instructions to show it to the astrologer Yen Chün-p'ing. When he returned, the astrologer recognised it as the shuttle of the Weaving Girl (Vega), and, moreover, said that at the time Zhang received the shuttle, he had seen a wandering star interpose itself between the Weaving Girl and the cow herd.^[97]

In Zoroastrianism, Vega was sometimes associated with Vanant, a minor divinity whose name means "conqueror".^[98]

The indigenous Boorong people of northwestern Victoria named it as Neilloan,^[99] "the flying Loan"^[100]

In Hindu mythology, Vega is called Abhijit.^[101] The author of Mahabharat, Maharshi Vyas, mentions in the chapter Vana Parva (Chap. 230, Verses 8–11): "Contesting against Abhijit (Vega), the constellation Krittika (Pleiades) went to "Vana" the Summer Solstice to heat the summer. Then the star Abhijit slipped down in the sky." P. V. Vartak suggests in his book, The Scholarly Dating of Mahabharat, that the "slipping of Abhijit" and ascension of Krittika (Pleiades) might refer to the gradual drop of Vega as a pole star since 12,000 BC. Vega is expected to become Earth's Pole star by year 26,000 by some estimates.^[102]

Medieval astrologers counted Vega as one of the Behenian stars^[103] and related it to chrysolite and winter savory. Cornelius Agrippa listed its kabbalistic sign under Vultur cadens, a literal Latin translation of the Arabic name.^[104] Medieval star charts also listed the alternate names Waghi, Vagieh and Veka for this star.^[42]

Vega became the first star to have a car named after it with the French Facel Vega line of cars from 1954 onwards, and later on, in America, Chevrolet launched the Vega in 1971.^[105] Other vehicles named after Vega include the ESA's Vega launch system^[106] and the Lockheed Vega aircraft.^[107]

Vega also featured prominently in Carl Sagan's novel, Contact. In the novel, the protagonists receive an interstellar message which appeared to have been transmitted from somewhere in the vicinity of Vega, leading to speculation that a planet orbiting Vega may have intelligent life.

See also

• Stars in astrology
• Vega in fiction

Notes

References

External links

Wikimedia Commons has media related to Vega.

• Anonymous, "Vega", SolStation (The Sol Company), retrieved 2005-11-09 
• Gilchrist, Eleanor et al. (2003-12-01), New evidence for Solar-like planetary system around nearby star, Joint Astronomy Centre, retrieved 2007-11-10 
• Hill, Gay Yee; Beasley, Dolores (2005-01-10), Spitzer Sees Dusty Aftermath of Pluto-Sized Collision, NASA/Spitzer Space Telescope, archived from the original on May 18, 2007, retrieved 2007-11-02 

Coordinates: 18^h 36^m 56.3364^s, +38° 47′ 01.291″

v t e Nearest star systems Star systems (including brown dwarf systems) within 30 light-years from Earth. v t e     0–5 ly → G V (Yellow) Solar System (0 ly; 1 star, 8 planets) Alpha Centauri (4.365 ± 0.007 ly; 3 stars: A B C (Proxima Centauri) (4.2421 ± 0.0016 ly); 1 planet: Bb) v t e ← 5–10 ly → A V (White) Sirius (8.60 ± 0.04 ly; 2 stars) M V (Red dwarf) Barnard's Star (5.979 ± 0.003 ly; 1 star) Wolf 359 (7.78 ± 0.04 ly; 1 star) Lalande 21185 (8.31 ± 0.01 ly; 1 star) Luyten 726-8 (8.73 ± 0.06 ly; 2 stars) Ross 154 (9.69 ± 0.06 ly; 1 star) Brown dwarf L Luhman 16 (6.58 ± 0.49 ly; 2 brown dwarfs) v t e ← 10–15 ly → F V (Yellow-white) Procyon (11.46 ± 0.05 ly; 2 stars) G V (Yellow) Tau Ceti (11.905 ± 0.007 ly; 1 star, 5? planets: b c d e f) K V (Orange) Epsilon Eridani (10.489 ± 0.005 ly; 1 star, 1 (2?) planets: b c) 61 Cygni (11.41 ± 0.02 ly; 2 stars) Epsilon Indi (11.81 ± 0.01 ly; 1 star, 2 brown dwarfs, 1? planets) M V (Red dwarf) Ross 248 (10.309 ± 0.018 ly; 1 star) Lacaille 9352 (10.68 ± 0.02 ly; 1 star) Ross 128 (10.94 ± 0.08 ly; 1 star) EZ Aquarii (11.27 ± 0.17 ly; 3 stars) Struve 2398 (11.64 ± 0.09 ly; 2 stars) Groombridge 34 (11.654 ± 0.025 ly; 2 stars) DX Cancri (11.83 ± 0.13 ly; 1 star) GJ 1061 (11.99 ± 0.06 ly; 1 star) YZ Ceti (12.12 ± 0.14 ly; 1 star) Luyten's Star (12.25 ± 0.03 ly; 1 star) Kapteyn's Star (12.76 ± 0.05 ly; 1 star) Lacaille 8760 (12.87 ± 0.04 ly; 1 star) Kruger 60 (13.05 ± 0.10 ly; 2 stars) Ross 614 (13.34 ± 0.05 ly; 2 stars) Wolf 1061 (14.00 ± 0.10 ly; 1 star) Gliese 1 (14.16 ± 0.06 ly; 1 star) Wolf 424 (14.31 ± 0.29 ly; 2 stars: A B) TZ Arietis (14.51 ± 0.19 ly; 1 star) Gliese 687 (14.77 ± 0.06 ly; 1 star) LHS 292 (14.81 ± 0.25 ly; 1 star) G 208-44/208-45 (14.81 ± 0.07 ly; 3 stars: A B G 208-45) Gliese 674 (14.81 ± 0.10 ly; 1 star, 1 planet: b) White dwarf DZ van Maanen's star (14.02 ± 0.11 ly; 1 star) Brown dwarf M Teegarden's star (12.57 ± 0.04 ly; 1 brown dwarf) SCR 1845-6357 (12.57 ± 0.05 ly; 2 brown dwarfs) DEN 1048-3956 (13.12 ± 0.06 ly; 1 brown dwarf) T WISE 1506+7027 (11.1+2.3 −1.3 ly; 1 brown dwarf) UGPS 0722-05 (13.43 ± 0.13 ly; 1 brown dwarf) Y WISE 0350-5658 (12.1+5.2 −1.3 ly; 1 brown dwarf) v t e ← 15–20 ly → A V (White) Altair (16.73 ± 0.05 ly; 1 star) G (Yellow) IV Delta Pavonis (19.92 ± 0.02 ly; 1 star) V Sigma Draconis «Alsafi» (18.77 ± 0.02 ly; 1 star) Eta Cassiopeiae «Achird» (19.42 ± 0.06 ly; 2 stars) e (82 G.) Eridani (19.71 ± 0.02 ly; 1 star, 3 planets: b c d) K V (Orange) Groombridge 1618 (15.89 ± 0.04 ly; 1 star) Omicron² (40) Eridani «Keid» (16.26 ± 0.02 ly; 3 stars) 70 Ophiuchi (16.58 ± 0.07 ly; 2 stars) Gliese 570 (19.00 ± 0.10 ly; 3 stars, 1 brown dwarf) 36 Ophiuchi (19.47 ± 0.07 ly; 3 stars) HR 7703 (19.62 ± 0.03 ly; 2 stars) M V (Red dwarf) Gliese 876 (15.21 ± 0.04 ly; 1 star, 4 planets: d c b e) GJ 1002 (15.31 ± 0.26 ly; 1 star) LHS 288 (15.55 ± 0.20 ly; 1 star) Gliese 412 (15.81 ± 0.08 ly; 2 stars) AD Leonis (15.94 ± 0.22 ly; 1 star) Gliese 832 (16.16 ± 0.08 ly; 1 star, 1 planet: b) EV Lacertae (16.46 ± 0.07 ly; 1 star) Gliese 682 (16.60 ± 0.20 ly; 1 star) GJ 1116 (17.06 ± 0.23 ly; 2 stars) GJ 3379 (17.10 ± 0.17 ly; 1 star) LHS 1723 (17.36 ± 0.12 ly; 1 star) Gliese 445 (17.42 ± 0.15 ly; 1 star) Wolf 498 (17.66 ± 0.07 ly; 1 star) Stein 2051 (18.07 ± 0.08 ly; 2 stars) Gliese 251 (18.31 ± 0.15 ly; 1 star) Gliese 205 (18.53 ± 0.11 ly; 1 star) L 449-1 (18.6 ± 3.9 ly; 1 star) LP 816-060 (18.63 ± 0.37 ly; 1 star) Gliese 229 (18.77 ± 0.11 ly; 1 star, 1 brown dwarf) Ross 47 (19.02 ± 0.11 ly; 1 star) Gliese 693 (19.06 ± 0.25 ly; 1 star) Gliese 752 (19.08 ± 0.06 ly; 2 stars: A B (vB 10)) Gliese 754 (19.28 ± 0.18 ly; 1 star) Gliese 588 (19.35 ± 0.15 ly; 1 star) GJ 1005 (19.37 ± 0.10 ly; 2 stars) Gliese 908 (19.41 ± 0.14 ly; 1 star) YZ Canis Minoris (19.51 ± 0.24 ly; 1 star) 2MASS J05332802-4257205 (~19.6 ly; 1 star) 2MASS J18450079-1409036 (~19.6 ly; 2 stars) Gliese 338 (19.92 ± 0.31 ly; 2 stars) Gliese 268 (19.96 ± 0.22 ly; 2 stars) White dwarf DQ LP 145-141 (15.09 ± 0.08 ly; 1 star) G 240-72 (19.80 ± 0.29 ly; 1 star) Brown dwarf M LP 944-020 (16.19 ± 0.35 ly; 1 brown dwarf) 2MASS 1835+3259 (18.48 ± 0.05 ly; 1 brown dwarf) L DEN 0255-4700 (16.20 ± 0.32 ly; 1 brown dwarf) T DEN 0817-6155 (16.1+1.1 −1.0 ly; 1 brown dwarf) WISE J0521+1025 (16.3 ± 4.2 ly; 1 brown dwarf) 2MASS 0939-2448 (17.41 ± 0.44 ly; 2 brown dwarfs) WISE 1741+2553 (18.1+1.6 −1.4 ly; 1 brown dwarf) 2MASS 1114-2618 (18.20 ± 0.14 ly; 1 brown dwarf) 2MASS 0415-0935 (18.62 ± 0.18 ly; 1 brown dwarf) 2MASS 0937+2931 (19.97 ± 0.20 ly; 1 brown dwarf) Y WISE 1639-6847 (16.3+1.8 −1.5 ly; 1 brown dwarf) WISE 0359-5401 (19.2+4.2 −2.6 ly; 1 brown dwarf) v t e ← 20–25 ly → G (Yellow) IV Beta Hydri (24.33 ± 0.02 ly; 1 star) V Xi Boötis (21.89 ± 0.07 ly; 2 stars) VI Mu Cassiopeiae (Marfak-West) (24.64 ± 0.15 ly; 2 stars) K V (Orange) HR 8832 (21.34 ± 0.04 ly; 1 star) HR 753 (23.42 ± 0.08 ly; 3 stars) Gliese 667 (23.60 ± 0.12 ly; 3 stars: A B C; 5 (7?) planets: Cb Ch? Cc Cf Ce Cd Cg?) HD 4628 (24.31 ± 0.09 ly; 1 star) 107 Piscium (24.57 ± 0.09 ly; 1 star) M V (Red dwarf) Gliese 784 (20.22 ± 0.13 ly; 1 star) HN Librae (20.29 ± 0.25 ly; 1 star) Gliese 581 (20.38 ± 0.21 ly; 1 star, 4 (6?) planets: e b c g? d f?) EQ Pegasi (20.40 ± 0.20 ly; 2 stars) LHS 2090 (20.8 ± 0.4 ly; 1 star) LHS 337 (20.8 ± 0.3 ly; 1 star) Furuhjelm 46 (20.9 ± 0.2 ly; 2 stars) G 180-060 (20.9 ± 0.6 ly; 1 star) V1054 Ophiuchi (21.05 ± 0.07 ly; 5 stars: Ba Bb A Gl 643 C (vB 8)) LP 71-82 (~21.2 ly; 1 star) G 161-71 (~21.3 ly; 1 star) Gliese 625 (21.3 ± 0.2 ly; 1 star) GJ 1128 (21.3 ± 0.4 ly; 1 star) GL Virginis (21.3 ± 0.4 ly; 1 star) LHS 3003 (21.4 ± 0.3 ly; 1 star) Gliese 408 (21.8 ± 0.3 ly; 1 star) SCR J1546−5534 (~21.9 ly; 1 star) Gliese 829 (21.9 ± 0.3 ly; 2 stars) G 41-14 (22.1 ± 0.3 ly; 3 stars) EE Leonis (22.2 ± 0.5 ly; 1 star) Gliese 880 (22.3 ± 0.2 ly; 2 stars) Gliese 299 (22.3 ± 0.5 ly; 1 star) LP 771-095 (22.7 ± 0.4 ly; 3 stars) GJ 1068 (22.7 ± 0.3 ly; 1 star) 2MASS J20360829-3607115 (~22.8 ly; 1 star) L 369-44 (~22.8 ly; 2 stars) 2MASS J18522528-3730363 (~22.8 ly; 1 star) G 161-7 (~22.8 ly; 2 stars) Gliese 809 (23.0 ± 0.1 ly; 2 stars) Gliese 393 (23.0 ± 0.4 ly; 1 star) Gliese 54 (23.1 ± 0.6 ly; 2 stars) SCR J0740−4257 (~23.5 ly; 1 star) L 43-72 (23.5 ± 4.9 ly; 1 star) GJ 1286 (23.6 ± 0.6 ly; 1 star) GJ 4063 (23.6+9.6 −5.3 ly; 1 star) GJ 4053 (23.7 ± 0.9 ly; 1 star) GJ 4274 (24.3 ± 0.9 ly; 1 star) GJ 3991 (24.28 ± 0.36 ly; 2 stars) GJ 4248 (24.29 ± 0.24 ly; 1 star) Gliese 109 (24.5 ± 0.4 ly; 1 star) GJ 1224 (24.6 ± 0.7 ly; 1 star) GJ 3378 (24.7 ± 0.5 ly; 1 star) Gliese 514 (24.97 ± 0.20 ly; 1 star) White dwarf DZ LP 658-2 (20.89 ± 0.11 ly; 1 star) Brown dwarf L 2MASS 1507-1627 (23.91 ± 0.11 ly; 1 brown dwarf) T 2MASS 1503+2525 (20.75 ± 0.29 ly; 1 brown dwarf) SIMP J013656.5+093347 (20.9 ± 1.0 ly; 1 brown dwarf) WISE 1928+2356 (~22.8 ly; 1 brown dwarf) WISE 0005+3737 (~23.2 ly; 1 brown dwarf) WISE 0049+2151 (~24.1 ly; 1 brown dwarf) WISE 0254+0223 (24.2+3.0 −2.4 ly; 1 brown dwarf) Y WISE 0146+4234 (~20.5 ly; 1 brown dwarf) WISE 2056+1459 (22.6+4.3 −3.1 ly; 1 brown dwarf) WISE 0713-2917 (~23.1 ly; 1 brown dwarf) WISE 0410+1502 (24.7+3.2 −2.5 ly; 1 brown dwarf) v t e ← 25–30 ly → A V (White) Vega (25.04 ± 0.07 ly; 1 star) Fomalhaut (25.13 ± 0.09 ly; 3 stars: A B (TW Piscis Austrini) (24.82 ± 0.12 ly) C (LP 876-10) (24.70 ± 0.22 ly); 1 planet: Ab) F V (Yellow-white) Pi³ Orionis «Tabit» (26.2 ± 0.2 ly; 1 star) Chi Draconis (26.22 ± 0.11 ly; 2 stars) Zeta Tucanae (28.0 ± 0.2 ly; 1 star) Gamma Leporis (29.3 ± 0.2 ly; 2 stars) G (Yellow) IV Mu Herculis (27.4 ± 0.2 ly; 4 stars) V Xi Ursae Majoris «Alula Australis» (27.25 ± 0.18 ly; 3 stars, 2 brown dwarfs) Beta Canum Venaticorum «Chara» (27.3 ± 0.2 ly; 1 star) 61 Virginis (27.8 ± 0.2 ly; 1 star, 3 planets: b c d) Chi¹ Orionis (28.3 ± 0.3 ly; 2 stars) 41 G. Arae (28.7 ± 0.3 ly; 2 stars) Beta Comae Berenices (29.9 ± 0.2 ly; 1 star) Kappa¹ Ceti (29.9 ± 0.2 ly; 1 star) VI Groombridge 1830 (29.9 ± 0.2 ly; 1 star) K (Orange) IV Delta Eridani «Rana» (29.49 ± 0.06 ly; 1 star) V Gliese 673 (25.12 ± 0.14 ly; 1 star) Gliese 884 (26.6 ± 0.3 ly; 1 star) p Eridani (26.57 ± 0.31 ly; 2 stars) Gliese 250 (28.4 ± 0.3 ly; 2 stars) HR 1614 (28.8 ± 0.3 ly; 1 star) HR 7722 (28.8 ± 0.3 ly; 1 star, 2 planets: b c) M V (Red dwarf) LHS 1070 (25.2 ± 0.5 ly; 3 stars) Gliese 701 (25.3 ± 0.3 ly; 1 star) GJ 1093 (25.3 ± 0.7 ly; 1 star) Gliese 480.1 (25.4 ± 0.8 ly; 1 star) SIPS 1259-4336 (25.4 ± 0.2 ly; 1 star) Gliese 382 (25.48 ± 0.30 ly; 1 star) DG Canum Venaticorum (25.9+5.5 −3.8 ly; 1 star) Wolf 922 (25.9 ± 0.5 ly; 2 stars) Gliese 300 (25.97 ± 0.20 ly; 1 star) SSSPM J1138-7722 (26 ± 3 ly; 1 star) Gliese 793 (26.08 ly; 1 star) 2MASS J12140866-2345172 (~26.1 ly; 1 star) 2MASS J19513587-3510375 (~26.1 ly; 1 star) SCR 0838-5855 (~26.1 ly; 1 star) Gliese 257 (26.2 ± 0.6 ly; 2 stars) Gliese 623 (26.2 ± 0.3 ly; 2 stars) GJ 1289 (26.4 ± 0.6 ly; 1 star) GJ 1105 (26.4 ± 0.7 ly; 1 star) Gliese 686 (26.5 ± 0.4 ly; 1 star) Gliese 493.1 (26.6 ± 1.0 ly; 1 star) Gliese 48 (26.6 ± 0.3 ly; 1 star) Gliese 747 (26.6 ± 0.4 ly; 2 stars) SCR 1138-7721 (26.7 ± 0.7 ly; 1 star) Gliese 486 (26.8 ± 0.6 ly; 1 star) GJ 1151 (26.8 ± 0.7 ly; 1 star) GJ 1227 (26.9 ± 0.4 ly; 1 star) GJ 1230 (27.0+1.7 −1.5 ly; 3 stars) Gliese 232 (27.2 ± 0.4 ly; 1 star) AP Columbae (27.4 ± 0.2 ly; 1 star) GJ 3146 (27.6 ± 1.7 ly; 1 star) GJ 1154 (27.6 ± 0.9 ly; 1 star) GJ 1057 (27.6 ± 0.9 ly; 1 star) Gliese 618 (27.6 ± 0.6 ly; 2 stars) GJ 3076 (27.6+6.0 −4.2 ly; 1 star) SCR 0640-0552 (~27.7 ly; 1 star) HD 32450 (27.8 ± 0.4 ly; 2 stars) Gliese 450 (27.9 ± 0.3 ly; 1 star) Gliese 877 (28.1 ± 0.3 ly; 1 star) Gliese 745 (28.1 ± 0.6 ly; 2 stars) Gliese 867 (28.2 ± 0.4 ly; 2 stars) GJ 3454 (28.2 ± 0.2 ly; 2 stars) SCR 0630-7643 (28.6 ± 0.5 ly; 2 stars) HU Delphini (28.6 ± 0.5 ly; 2 stars) LDS 169 (28.6 ± 0.8 ly; 2 stars) Gliese 849 (28.6 ± 0.5 ly; 1 star, 2 planets: b c) GJ 1103 (28.7 ± 0.8 ly; 2 stars) GJ 1207 (28.8 ± 0.4 ly; 1 star) Gliese 465 (29.0 ± 0.7 ly; 1 star) GJ 1277 (29.0 ± 4.6 ly; 1 star) GJ 3128 (29.1 ± 0.5 ly; 1 star) V374 Pegasi (29.1 ± 0.9 ly; 1 star) Gliese 357 (29.3 ± 0.5 ly; 1 star) Gliese 595 (29.4 ± 3.5 ly; 1 star) Gliese 433 (29.5 ± 0.5 ly; 1 star, 2 planets: b c) Gliese 424 (29.7 ± 0.3 ly; 1 star) GJ 3801 (29.7 ± 0.9 ly; 1 star) GJ 2066 (29.9 ± 0.5 ly; 1 star) LHS 224 (29.9 ± 0.8 ly; 2 stars) SCR 1826-6542 (~30 ly; 1 star) White dwarf DA G 99-47 (26.1 ± 0.8 ly; 1 star) WD 2359-434 (26.7 ± 0.3 ly; 1 star) Gliese 318 (28.7 ± 0.5 ly; 1 star) DC L 97-12 (25.83 ± 0.27 ly; 1 star) DQ LHS 1126 (29.5 ± 0.3 ly; 1 star) DZ Wolf 489 (26.9 ± 0.8 ly; 1 star) LP 701-29 (27.9 ± 0.2 ly; 1 star) L 745-46 (29.7 ± 0.2 ly; 2 stars) Brown dwarf M DENIS 0334-49 (27.04 ± 0.83 ly; 1 brown dwarf) GJ 3517 (27.8 ± 0.4 ly; 1 brown dwarf) L WISE 0607+2429 (25.4+4.6 −3.9 ly; 1 brown dwarf) 2MASS 0835-08 (27.9+2.9 −2.4 ly; 1 brown dwarf) WISE 1647+5632 (28.1+9.4 −5.6 ly; 1 brown dwarf) 2MASS 0036+1821 (28.6 ± 0.2 ly; 1 brown dwarf) WISE 1800+0134 (28.7 ± 3.3 ly; 1 brown dwarf) 2MASS J04390101-2353083 (29.5 ± 1.1 ly; 1 brown dwarf) SDSS J1416+1348 (29.7 ± 0.3 ly; 2 brown dwarfs) 2MASS J16452211-1319516 (29.7 ± 1.7 ly; 1 brown dwarf) 2MASS J03552337+1133437 (29.8+0.4 −0.3 ly; 1 brown dwarf) T 2MASS 0348-6022 (~25.4 ly; 1 brown dwarf) 2MASS 0729-39 (25.8 ± 1.8 ly; 1 brown dwarf) UGPS J0521+3640 (26.7+3.9 −3.2 ly; 1 brown dwarf) WISE 0313+7807 (~28.0 ly; 1 brown dwarf) 2MASS 0727+1710 (29.0 ± 0.2 ly; 1 brown dwarf) Y WISE 1405+5534 (25.3+4.4 −3.2 ly; 1 brown dwarf) WISE 2220-3628 (~26.4 ly; 1 brown dwarf) WISE 0647-6232 (28.4+3.3 −2.7 ly; 1 brown dwarf) In left column are stellar classes of primary members of star systems. Bold are systems containing at least one component with absolute magnitude of +8.5 or brighter. Italic are systems without known trigonometric parallax.

v t e Stars of Lyra Bayer α (Vega) β (Sheliak) γ (Sulafat) δ1 δ2 ε1, 2 (Double Double) ζ1 ζ2 η (Aladfar) θ ι κ λ μ (Alathfar) ν1 ν2 Flamsteed 16 17 19 Variable R (13) S T V W RR RV RZ TT TZ UZ XY AY CC CN CY DM EP EZ FL HK HP HR KX MV V344 V361 V404 V473 V477 V478 V533 V542 V543 V545 V550 V558 HR 6845 6847 6853 6901 6968 6984 6997 7016 7017 7019 7030 7033 7041 7043 7044 7064 7073 7081 7112 7115 7118 7132 7140 7146 7162 7181 7202 7204 7212 7237 7238 7244 7253 7272 7280 7284 7302 7338 7345 7346 7359 7376 7382 HD 177830 180314 181068 Gliese Gliese 758 GJ 4063 Other GSC 02634-01087 GSC 02652-01324 Kepler-7 Kepler-8 Kepler-9 Kepler-12 Kepler-14 Kepler-19 Kepler-20 Kepler-24 Kepler-25 Kepler-26 Kepler-30 Kepler-33 Kepler-37 Kepler-38 Kepler-53 Kepler-55 Kepler-59 Kepler-60 Kepler-62 Kepler-65 Kepler-80 Kepler-88 Kepler-102 2MASS 1835+3259 WASP-3 WASP-58 WISE 1828+2650 List