Vega, Alpha Lyrae (α Lyr), is a bright white main sequence star located only 25 light years from Earth. With an apparent magnitude of 0.026, it is the brightest star in the constellation Lyra and the fifth brightest star in the sky, after Sirius, Canopus, Alpha Centauri and Arcturus. Vega is also the second brightest star in the northern celestial hemisphere, slightly fainter only than Arcturus and just outshining Capella.
Vega has the spectral classification A0V, indicating a white star on the main sequence, still fusing hydrogen to helium in its core. The star has more than twice the Sun’s mass and radius. With a surface temperature of 9,600 K, it shines with 40 solar luminosities. Its estimated age is about 455 million years.
Even though it is only about a tenth the age of the Sun, having twice its mass means that it will also live only a tenth of the Sun’s lifetime. These days, Vega is close to the midpoint of its life cycle. It will become an M-type red giant in about 500 million years, after it stops fusing hydrogen in its core, and eventually lose most of its mass and evolve into a white dwarf.
Vega is a suspected Delta Scuti variable star, one whose variations in luminosity result from both radial and non-radial pulsations of its surface. Also known as dwarf Cepheids, these stars are used as standard candles to establish distances to open and globular star clusters, galaxies, and the Galactic centre.
Vega completes a full rotation around its axis every 12.5 hours. For comparison, the Sun takes just over 25 days even though it is considerably smaller. As a result of the star’s high rotational velocity – estimates are as high as 236.2 ± 3.7 km/s along the equator – there is flattening at its poles and its equator is extended, giving Vega the shape of an oblate spheroid. The star is 23 percent wider at the equator than at the poles. Its equatorial bulge cannot be observed directly because we only get a pole-on view. If we could see Vega from its equatorial plane, its spectrum would be about half as luminous because the temperature is lower at the equator than at the poles and there is a circumstellar debris ring around the equator, where planets may be formed, that would block some of the star’s light. No planets have been detected around Vega so far. Even if they exist, the star’s short life span makes it unlikely that any complex form of life could develop there.
The star’s ellipsoid shape means that gravity at the equator is lower than at the poles because the centre of mass is further away at the equator. Gravity affects the amount of energy the star radiates and, as a result, there is a significant difference in surface temperature between the poles and the equator. The temperature at the poles is about 17,900° F, while the equatorial surface temperature is only 13,800° F. This phenomenon is known as gravity darkening. The poles are said to be “gravity brightened,” while the equator is “gravity darkened.” Achernar, the brightest star in Eridanus constellation, is another example of this.
In 1997, the James Clerk Maxwell Telescope discovered a bright central region about 9’’ northeast of Vega, appearing as an irregularity in the star’s dust disk. Astronomers have hypothesized that this indicates the presence of a planet. In 2005, they narrowed down the size of the hypothetical planet to 5-10 times the mass of Jupiter. However, two years later, observations with the Plateau de Bure Interferometer revealed a smooth and symmetric debris disk, without any evidence of the previously reported irregularities. Observations with the Herschel Space Telescope in 2012 confirmed the smooth structure of the disk. Even though there is no evidence of a massive planet, there still may be smaller planets orbiting Vega at a closer distance, where they are more difficult to detect.
An observer on a planet orbiting Vega would see the Sun as a star with a visual magnitude of 4.3 located in the constellation Columba, the Dove.
Vega’s proximity and brightness have made the star a frequent object of study. It was one of the first stars to have its distance measured using parallax and the first star outside our solar system to be photographed. It was also the first star to have its spectrum measured.
Vega was first photographed using a 15-inch refractor telescope and the daguerreotype process on July 17, 1850 by William Bond and John Adams Whipple at the Harvard College Observatory. The star’s spectrum was first imaged by Henry Draper in August 1872. Draper was the first to reveal absorption lines in a star’s spectrum.
The German-Russian astronomer Friedrich Georg Wilhelm von Struve was the first to measure Vega’s parallax. He gave a value of 0.125 arcseconds, but later revised it, almost doubling the original estimate, after German astronomer and physicist Friedrich Bessel had expressed doubts regarding the data. Struve’s original result was closer to the currently accepted number of 0.129’’, as measured by the Hipparcos satellite, but as a result of Struve’s revision, it was Bessel who was credited for publishing the first stellar parallax (0.314’’ for 61 Cygni).
Vega is used as a zero point for the colour index, the numerical expression that determines the colour of an astronomical object. Stars that are hotter and bluer than Vega have a smaller colour index, while those that are redder and cooler have a larger one. Vega’s U-B and B-V colour index is set at 0.00.
Vega’s brightness is still used to define zero magnitude for the visible and near infrared parts of the spectrum, with small adjustments. The zero point was originally established by assigning Polaris a magnitude of 2.00, but once astronomers discovered that the North Star was variable, they settled on Vega as the reference star. This is why the Sun, the four other stars that are brighter than Vega – Sirius, Canopus, Alpha Centauri and Arcturus – as well as the planets Venus, Mars and Jupiter, have negative magnitudes.
From Earth, Vega is seen from the direction of one of its poles. For this reason, its projected rotational velocity is much lower (just above 20 km/s) than more recent measurements indicate. The star is in fact a very fast spinner, rotating at about 90% of its breakup velocity, with estimates of its rotation velocity as high as 236.2 km/s at the equator.
Vega’s variability was detected in the 1930s, when photometric measurements revealed changes in its brightness on the order of ±0.03 magnitudes. Measurements in 1981 indicated low-amplitude pulsations characteristic of a Delta Scuti-type star.
In 1979, observations with an X-ray telescope revealed that Vega was an X-ray emitter. At the time, Vega was the only main sequence star beyond the Sun known to be an X-ray source.
In 1983, the Infrared Astronomical Satellite (IRAS) detected an excess of infrared radiation coming from Vega. This indicated the presence of a circumstellar disk of dust. Vega was the first star known to have one. The disk extends for hundreds of astronomical units. High-resolution images of the dust were produced by the Spitzer Space Telescope in 2005. Observations with the Palomar Testbed Interferometer in 2001, the CHARA array in 2006, and the Infrared Optical Telescope Array in 2011 showed evidence of an inner dust band around the star.
Vega was also the first class A star (that is not Ap chemically peculiar) known to have a magnetic field and, in 2015, it became the first normal class A star known to have star spots on its surface.
Vega has an unusually low metallicity and observations suggest that it is a weak Lambda Boötis star, a chemically peculiar star with a very low abundance of iron peak elements in its surface layers. There is no clear explanation for the existence of such stars.
Vega’s proper motion is slowly taking the star toward Earth. It will make its closest approach in about 264,000 years, when it comes within 13.2 light years (4.04 parsecs). Around the year 210000 CE, it will take over from Sirius as the brightest star in the sky. It will lie at a distance of 17.2 light years and shine at magnitude -0.81.
Vega is one of the 58 bright stars that have been given a special status in the field of celestial navigation. Navigational stars are some of the brightest and most recognizable stars in the sky. Polaris, Deneb and Altair are also included on the list.
Vega was the North Pole star around 12000 BCE and will be again around 13700 CE, when precession of the equinoxes takes it within 5° of true north. It was and will be the Earth’s brightest North Star. Polaris (Alpha Ursae Minoris), the current North Star, is only the 48th brightest star.
Vega is associated with the Lyrids, a meteor shower that can be seen from April 16 to April 26 each year, peaking around April 22 with 5 to 10 meteors per hour. The radiant of the Lyrid meteor shower is located near the star, but this is just a line-of-sight coincidence. The true source of the meteor shower is the long-period Comet C/1861 G1 Thatcher, and the particles of dust left behind by the comet that burn up in the Earth’s atmosphere are only about 100 km away.
In medieval astrology, Vega was considered one of the Behenian fixed stars, 15 stars believed to be a source of astrological power for one or more planets and considered useful for magical applications. Vega was associated with Mercury and Venus and linked to winter savory and chrysolite. Astrologers believed that it gave artistic talent, aspirations for status and influence, high success, refinement, and a tendency for debauchery.
Like most exceptionally bright stars, Vega has been used or referenced in countless works of fiction. The best known ones include Foundation (1951) by Isaac Asimov, Alfred Bester’s The Stars My Destination (1956), Robert A. Heinlein’s Have Space Suit – Will Travel (1958), Roger Zelazny’s This Immortal (1966), Carl Sagan’s Contact (1985), Dan Simmons’ Hyperion (1989) and The Fall of Hyperion (1990), and Greg Egan’s Diaspora (1997).
The name Vega (once also spelled Wega) derives from the Arabic wāqi‘, which means “falling” or “landing.” It was taken from the phrase an-nasr al-wāqi‘, “the falling eagle.” The name was officially approved for Alpha Lyrae by the International Astronomical Union’s (IAU) Working Group on Star Names (WGSN) on June 30, 2016.
The star’s Arabic name appeared in Egyptian astronomer Mohammad Al Achsasi Al Mouakket’s star catalogue, written circa 1650, and was later translated into Latin as Vultur Cadens, meaning “the falling eagle (or vulture).” Lyra constellation was depicted as a vulture by ancient Egyptians and was similarly represented as a vulture or eagle in ancient India.
In the western world, the name appeared in the Alfonsine Tables, compiled in Spain in the mid-13th century. Medieval astrolabes (inclinometers used to measure stars’ altitude above the horizon) in Europe depicted the star as a bird and called it Wega or Alvaca.
The Chinese name for Vega is the First Star of Weaving Girl (織女一), referring to the asterism known as the Weaving Girl, formed by Vega with Epsilon Lyrae and Zeta1 Lyrae. In Chinese lore, Vega and Altair are associated with the myth of Qixi (Qi means “seven” and Xi means “night”) and the Qixi Festival (Seventh Evening Festival). The festival is traditionally held on the seventh day of the seventh month on the Chinese lunar calendar to celebrate the annual meeting of Niulang (the cowherd, represented by Altair) and Zhinü (the weaver girl, represented by Vega). In the story, the two lovers are separated by a large river, represented the Milky Way, and can only meet once a year, when magpies create a bridge so that they can briefly be together again.
The legend is more than 2,600 years old. It also inspired the Tanabata festival in Japan and the Chilseok festival in Korea. The Tanabata festival celebrates the meeting of Orihime (Vega) and Hikoboshi (Altair), while the Korean event is associated with the folktale of Jiknyeo (the weaver girl) and Gyeonwu (the herder).
To the ancient Greeks, the star symbolized the handle of Orpheus’ harp, while the Romans based the start of the autumn season on the hour of Vega’s falling below the horizon. The Assyrians called the star Dayan-same, meaning “the judge of heaven,” and Akkadians knew it as Tir-anna, or “life of heaven”. In ancient Babylonian culture, Vega may have been one of the stars known as Dilgan, or “the messenger of light.” In Hindu mythology, the star is known as Abhijit, meaning “the victorious one” or “the undefeatable one.” In the Mahabharata, Krishna says that he was born under this nakshatra (lunar mansion associated with the star).
In northern Polynesia, Vega was known as whetu o te tau, which means “the year star”. It once marked the beginning of the new year, before the function was assigned to the Pleiades cluster.
In northwest Victoria in Australia, the Boorong people called Vega Neilloan, or “the flying loan,” referring to the ground-dwelling Australian malleefowl. The Lyrids represented the scratchings of the malleefowl during the nest-building season.
Vega is relatively easy to find because it lies at the northwest vertex of the Summer Triangle, a bright, large asterism that dominates the evening sky during the northern hemisphere summer. The other two stars that form the asterism are Deneb, the brightest star in Cygnus, the Swan, and also part of the Northern Cross asterism, and Altair, the brightest star in Aquila, the Eagle, located opposite Cygnus.
Vega is circumpolar north of latitude 51°N and can be seen throughout the year. It is visible from all locations north of latitude 51°S. From mid-northern latitudes, the star can be seen near the zenith in the evening during the northern hemisphere summer, while observers in mid-southern latitudes can see it low above the northern horizon during the southern winter months.
Vega is located in the constellation Lyra. Lyra is a relatively small constellation, sandwiched between the larger Cygnus and Hercules, and Vega stands out in this part of the sky as the brightest of the stars that form the constellation’s distinctive lyre-shaped asterism. Sulafat, Lyra’s second brightest star, is considerably fainter, with a visual magnitude of 3.261.
Lyra represents the lyre of the mythical Greek musician and poet Orpheus. The constellation is a popular telescope target because, despite its size, it contains several interesting stars and deep sky objects. Notable stars in the constellation include the variable stars Beta Lyrae, R Lyrae and RR Lyrae, the visual double Delta Lyrae, and the multiple star system Epsilon Lyrae, also known as the Double Double.
Interesting deep sky objects in Lyra include the planetary nebula Messier 57 (Ring Nebula), the bright globular cluster Messier 56, the open cluster NGC 6791 and the interacting triplet of galaxies designated as NGC 6745.
The best time of year to see the stars and deep sky objects in Lyra is during the month of August, when the constellation is high overhead in the evening for northern observers.
The 10 brightest stars in Lyra are Vega (Alpha Lyrae, mag. 0.026), Sulafat (Gamma Lyrae, mag. 3.261), Sheliak (Beta Lyrae A, mag. 3.52), R Lyrae (mag. 4.00), Delta2 Lyrae (mag. 4.22), Kappa Lyrae (mag. 4.35), Zeta1 Lyrae (mag. 4.34), Theta Lyrae (mag. 4.347), Aladfar (Eta Lyrae, mag. 4.40), and Epsilon2 Lyrae A (mag. 4.59).
Vega – Alpha Lyrae
|Spectral class||A0 Va|
|Variable type||Delta Scuti|
|U-B colour index||0.00|
|B-V colour index||0.00|
|Apparent magnitude||+0.026 (-0.02 to +0.07)|
|Distance||25.04 ± 0.07 light years (7.68 ± 0.02 parsecs)|
|Parallax||130.23 ± 0.36 mas|
|Radial velocity||−13.9 ± 0.9 km/s|
|Proper motion||RA: 200.94 mas/yr|
|Dec.: 286.23 mas/yr|
|Mass||2.135 ± 0.074 M☉|
|Luminosity||40.12 ± 0.45 L☉|
|Radius||2.362 × 2.818 R☉|
|Temperature||9,602 ± 180 K|
|Age||455 million years|
|Rotational velocity||20.48 ± 0.11 km/s (up to 236.2 ± 3.7 km/s at the equator)|
|Surface gravity||4.1 ± 0.1 cgs|
|Right ascension||18h 36m 56.33635s|
|Declination||+38° 47′ 01.2802”|
|Designations||Vega, Alpha Lyrae, α Lyr, 3 Lyrae, Wega, HIP 91262, HD 172167,HR 7001, SAO 67174, BD+38°3238, GJ 721, LTT 15486, GCTP 4293.00, CCDM J18369+3847A, 2MASS J18365633+3847012, TYC 3105-2070-1|