Beta Lyrae
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Lyra |
Right ascension | 18h 50m 04.79525s[1] |
Declination | +33° 21′ 45.6100″[1] |
Apparent magnitude (V) | 3.52[2] (3.25 – 4.36[3]) |
Characteristics | |
Spectral type | B6-8II[4][5] + B[2] |
U−B color index | −0.56[6] |
B−V color index | +0.00[6] |
Variable type | |
Astrometry | |
A | |
Radial velocity (Rv) | −19.2[7] km/s |
Proper motion ( | RA: 1.90[1] mas/yr Dec.: −3.53[1] mas/yr |
Parallax ( | 3.39 ± 0.17 mas[1] |
Distance | 960 ± 50 ly (290 ± 10 pc) |
Absolute magnitude (MV) | −3.82[8] |
B | |
Radial velocity (Rv) | −14±5[9] km/s |
Proper motion ( | RA: 4.373±0.087[10] mas/yr Dec.: −0.982±0.098[10] mas/yr |
Parallax ( | 3.0065 ± 0.0542 mas[10] |
Distance | 1,080 ± 20 ly (333 ± 6 pc) |
Orbit[2] | |
Primary | Aa1 |
Companion | Beta Lyrae Aa2 |
Period (P) | 12.9414 days |
Semi-major axis (a) | 0.865±0.048 mas |
Eccentricity (e) | 0 |
Inclination (i) | 92.25 ± 0.82° |
Longitude of the node ( | 254.39 ± 0.83° |
Details[11] | |
Mass | 2.97 ± 0.2 M☉ |
Radius | 15.2 ± 0.2 R☉ |
Luminosity | 6,500 L☉ |
Surface gravity (log g) | 2.5 ± 0.1 cgs |
Temperature | 13,300 K |
Age | 23 Myr |
Mass | 13.16 ± 0.3 M☉ |
Radius | 6.0 ± 0.2 R☉ |
Luminosity | 26,300 L☉ |
Surface gravity (log g) | 4.0 ± 0.1 cgs |
Temperature | 30,000 ± 2,000 K |
Other designations | |
Database references | |
SIMBAD | |
B |
Beta Lyrae (
Although it appears as a single point of light to the naked eye, it actually consists of six components of apparent magnitude 14.3 or brighter. The brightest component, designated Beta Lyrae A, is itself a triple star system, consisting of an eclipsing binary pair (Aa) and a single star (Ab). The binary pair's two components are designated Beta Lyrae Aa1 and Aa2. The additional five components, designated Beta Lyrae B, C, D, E, and F, are currently considered to be single stars.[12][13][14][15][16][17]
Nomenclature[edit]
Beta Lyrae bore the traditional name Sheliak (occasionally Shelyak or Shiliak), derived from the Arabic الشلياق šiliyāq or Al Shilyāk, one of the names of the constellation of Lyra in Islamic astronomy.[19] Notably, in Arabic sources the Lyra constellation is primarily referred to as سِلْيَاق (Romanization: Siliyāq),[20][21] whereas شلياق (Šiliyāq) primarily is used to refer to Beta Lyrae in what might be a form of linguistic reborrowing.[22][23] Persian sources on the other hand, do refer to the Lyra constellation as شلياق (Šiliyāq), which may be the source of this confusion.[24][25]
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[26] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[27] It approved the name Sheliak for the component Beta Lyrae Aa1 on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.[28]
In Chinese astronomy, Tsan Tae (
Properties[edit]
![](https://upload.wikimedia.org/wikipedia/commons/thumb/0/04/Beta_Lyrae_-_CHARA.gif/220px-Beta_Lyrae_-_CHARA.gif)
Beta Lyrae Aa is a semidetached binary system made up of a stellar class B6-8 primary star and a secondary that is probably also a B-type star. The fainter, less massive star in the system was once the more massive member of the pair, which caused it to evolve away from the main sequence first and become a giant star. Because the pair are in a close orbit, as this star expanded into a giant it filled its Roche lobe and transferred most of its mass over to its companion.
The secondary, now more massive star is surrounded by an accretion disk from this mass transfer, with bipolar, jet-like features projecting perpendicular to the disk.[2] This accretion disk blocks humans' view of the secondary star, lowering its apparent luminosity and making it difficult for astronomers to pinpoint what its stellar type is. The amount of mass being transferred between the two stars is about 2 × 10−5 solar masses per year, or the equivalent of the Sun's mass every 50,000 years, which results in an increase in orbital period of about 19 seconds each year. The spectrum of Beta Lyrae shows emission lines produced by the accretion disc. The disc produces around 20% of the brightness of the system.[2]
In 2006, an adaptive optics survey detected a possible third companion, Beta Lyrae Ab. It was detected at 0.54" angular separation with a differential magnitude of +4.53. The difference in magnitudes suggests its spectral class is in the range B2-B5 V. This companion would make Beta Lyrae A a hierarchical triple system.[30]
Variability[edit]
![](https://upload.wikimedia.org/wikipedia/commons/thumb/a/ae/BetaLyrLightCurve.png/220px-BetaLyrLightCurve.png)
The variable luminosity of this system was discovered in 1784 by the British amateur astronomer John Goodricke.[32] The orbital plane of this system is nearly aligned with the line of sight from the Earth, so the two stars periodically eclipse each other. This causes Beta Lyrae to regularly change its apparent magnitude from +3.2 to +4.4 over an orbital period of 12.9414 days. It forms the prototype of a class of ellipsoidal "contact" eclipsing binaries.[3]
The two components are so close together that they cannot be resolved with optical telescopes, forming a spectroscopic binary. In 2008, the primary star and the accretion disk of the secondary star were resolved and imaged using the CHARA Array interferometer[33] and the Michigan InfraRed Combiner (MIRC)[34] in the near infrared H band (see video below), allowing the orbital elements to be computed for the first time.[2]
In addition to the regular eclipses, the system shows smaller and slower variations in brightness. These are thought to be caused by changes in the accretion disc and are accompanied by variation in the profile and strength of spectral lines, particularly the emission lines. The variations are not regular but have been characterised with a period of 282 days.[35]
Companions[edit]
In addition to Beta Lyrae A, several other companions have been catalogued.
The next two brightest components are E and F.
The Washington Double Star Catalog lists two fainter companions, C and D, at 47" and 64" separation, respectively.[39] Component C has been observed to vary in brightness by over a magnitude, but the type of variability is not known.[40]
Components A, B, and F are thought to be members of a group of stars around
The Gaia spacecraft has provided these data for the stars listed in the WDS:
Component[41] | Spectral Class | Magnitude (G) | Proper Motion | Radial Velocity (km/s) | Parallax (mas) | Simbad | |
---|---|---|---|---|---|---|---|
RA (mas/yr) | |||||||
A[42][a] | 3.25 – 4.36 | 1.569 ± 0.582 | -2.523 ± 0.594 | 2.20 ± 0.7 | 1.0851 ± 0.3398 | [12] | |
B[10] | B7V | 7.19 | 4.373 ± 0.087 | -0.982 ± 0.098 | -14 ± 5 | 3.0065 ± 0.0542 | [13] |
C[43] | B2 | 13.07 | -1.936 ± 0.024 | -1.824 ± 0.030 | ? | 0.2384 ± 0.0151 | [14] |
D[44] | K3V | 14.96 | -0.108 ± 0.062 | -17.792 ± 0.074 | ? | 0.8378 ± 0.0368 | [15] |
E[45] | G5 | 9.77 | 1.649 ± 0.051 | 0.719 ± 0.053 | 1.4 | 1.6209 ± 0.0339 | [16] |
F[46] | G5 | 10.10 | 1.258 ± 0.047 | -3.793 ± 0.052 | -16.83 ± 1.41 | 3.5222 ± 0.0307 | [17] |
References[edit]
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- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
External links[edit]
- Kaler, James B. (2002), The hundred greatest stars, Copernicus Series, Springer, p. 29, ISBN 978-0-387-95436-3
- Philippe Stee's homepage: Hot and Active Stars Research
- Kaler, James B., "SHELIAK (Beta Lyrae)", Stars, University of Illinois, retrieved 2011-12-20
- Bruton, Dan; Linenschmidt, Robb; Schmude, Jr., Richard W., Watching Beta Lyrae Evolve, Texas A&M University, archived from the original on 2003-02-25, retrieved 2011-12-20
- Beck, Sara J. (July 1, 2011), Beta Lyrae, AAVSO, retrieved 2011-12-20