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 atriple star system, consisting of aneclipsing 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]
β Lyrae (Latinised toBeta Lyrae) is the system'sBayer designation, established byJohann Bayer in hisUranometria of 1603, and denotes that it is the second brightest star in theLyra constellation. WDS J18501+3322 is a designation in theWashington Double Star Catalog. The designations of the constituents asBeta Lyrae A,B andC, or alternativelyWDS J18501+3322A,B andC, and additionallyWDS J18501+3322D,E andF, and those ofA's components -Aa1,Aa2 andAb - derive from the convention used by the Washington Multiplicity Catalog (WMC) formultiple star systems, and adopted by theInternational Astronomical Union (IAU).[18]
Beta Lyrae bore the traditional nameSheliak (occasionallyShelyak orShiliak), derived from theArabic الشلياقšiliyāq orAl Shilyāk, one of the names of the constellation ofLyra inIslamic 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 linguisticreborrowing.[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, theInternational Astronomical Union organized aWorking 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 entiremultiple systems.[27] It approved the nameSheliak 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]
Beta Lyrae Aa is asemidetached binary system made up of astellar 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 themain sequence first and become agiant star. Because the pair are in a close orbit, as this star expanded into a giant it filled itsRoche lobe and transferred most of its mass over to its companion.
The secondary, now more massive star is surrounded by anaccretion disk from this mass transfer, withbipolar, 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 about2 × 10−5solar 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. Thespectrum 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]
Thevariable luminosity of this system was discovered in 1784 by the British amateur astronomerJohn Goodricke.[32] In 1894,Aristarkh Belopolsky identified Beta Lyrae as an eclipsing spectroscopic binary.[33] The orbital plane of this system is nearly aligned with the line of sight from the Earth, so the two stars periodicallyeclipse each other. This causes Beta Lyrae to regularly change itsapparent 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 aspectroscopic binary. In 2008, the primary star and the accretion disk of the secondary star were resolved and imaged using theCHARA Array interferometer[34] and the Michigan InfraRed Combiner (MIRC)[35] 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.[36]
The date of a primary minimum can be calculated according the following formula:
In addition to Beta Lyrae A, several other companions have been catalogued. β Lyr B, at an angular separation of 45.7", is of spectral type B7V, has an apparent magnitude of +7.2, and can easily be seen with binoculars. It is about 80 times as luminous as the Sun. In 1962 it was identified as spectroscopic binary with a period of 4.348 days,[37] but the 2004 release of the SB9 catalog of Spectroscopic Binary Orbits omitted it, so it is now considered a single star.[13]
The next two brightest components are E and F. β Lyr E is magnitude 10.1v, separation 67", and β Lyr F is magnitude 10.6v, separation 86". Both arechemically peculiar stars;[38] both are catalogued asAp stars, although component F is sometimes thought to be anAm star.[39]
TheWashington Double Star Catalog lists two fainter companions, C and D, at 47" and 64" separation, respectively.[40] Component C has been observed to vary in brightness by over a magnitude, but the type of variability is not known.[41]
Components A, B, and F are thought to be members of a group of stars around β Lyrae, at approximately the same distance and moving together. The others just happen to be in the same line of sight.[39] Analysis ofGaia Data Release 2 astrometry reveals a group of about 100 stars around β Lyrae which share its space motion and are at the same distance. This cluster has been named Gaia 8. The cluster members are allmain sequence stars and the lack of a main sequence turnoff means that a precise age cannot be calculated, but the cluster age is estimated at 30 to 100 million years. The average Gaia DR2 parallax for the member stars is3.4 mas.[4]
TheGaia spacecraft has provided these data for the stars listed in the WDS:
^abcSamus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)".VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S.1.Bibcode:2009yCat....102025S.
^Evans, D. S. (1967). "The Revision of the General Catalogue of Radial Velocities".Determination of Radial Velocities and Their Applications.30: 57.Bibcode:1967IAUS...30...57E.
^Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets".arXiv:1012.0707 [astro-ph.SR].
^"معرفی و رصد صورت فلکی شلیاق و ستاره ی نسرواقع" [Introducing and observing a loose constellation and a real star.].موسسه علمی پژوهشی نجم شمال (in Persian). North Star Scientific Research Institute. Archived fromthe original on 2024-01-29. Retrieved2024-01-29.
^Abt, Helmut A.; Jeffers, Hamilton M.; Gibson, James; Sandage, Allan R. (September 20, 1961). "The Visual Multiple System Containing Beta Lyrae".The Astrophysical Journal.135: 429.Bibcode:1962ApJ...135..429A.doi:10.1086/147282.
^Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)".VizieR On-line Data Catalog.Bibcode:2014yCat....1.2023S.
^Proust, D.; Ochsenbein, F.; Pettersen, B. R. (1981). "A catalogue of variable-visual binary stars".Astronomy and Astrophysics Supplement Series.44: 179.Bibcode:1981A&AS...44..179P.
