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사용자:Ta183ta/연습장: 두 판 사이의 차이

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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.
 
현 시점에서 주성보다 질량이 큰 반성은 The secondary, now more massive star is surrounded by an [[accretion disk]] from this mass transfer, with [[bipolar jets|bipolar, jet-like features]] projecting perpendicular to the disk.<ref name=apj684_2_L95/> 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 {{nowrap|2 × 10<sup>−5</sup> }}[[solar mass]]es 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 [[stellar spectrum|spectrum]] of Beta Lyrae shows emission lines produced by the accretion disc. The disc produces around 20% of the brightness of the system.<ref name=apj684_2_L95/>
 
==밝기 변화==
104번째 줄:
 
==동반 천체==
거문고자리 베타 외에 동반 천체 여럿도 천체목록에 실렸다. 거문고자리 베타 B는 각거리상으로 주성으로부터 45.7" 떨어져 있으며 분광형은 B7 V에 겉보기 등급은 +7.2이고 쌍안경으로 쉽게 볼 수 있다. B의 광도는 태양의 약 80 배이다. B는 1962년 공전주기 4.348 일의 분광쌍성으로 인식되었으나<ref>{{cite journal|date=September 20, 1961|author1= Abt, Helmut A. | author2=Jeffers, Hamilton M. |author3=Gibson, James |author4=Sandage, Allan R.|title=The Visual Multiple System Containing Beta Lyrae|journal= The Astrophysical Journal |volume= 135 |pages= 429 |bibcode= 1962ApJ...135..429A|doi=10.1086/147282}}</ref> but the 2004 release of the SB9 catalog분광쌍성궤도목록(Catalog of Spectroscopic Binary Orbits)의 omitted2004년 it, soSB9 it판에서 is거문고자리 now베타가 considered삭제되었기에 a지금은 single단독성으로 star여겨진다.<ref name="SIMBADB" />
 
The다음으로 next밝은 two동반 brightest천체들은 components거문고자리 are베타 EE와 and FF이다. βE의 Lyr겉보기 E is magnitude등급은 10.1v, separation각거리는 67",이며 andF의 β겉보기 Lyr F is magnitude등급은 10.6v, separation각거리는 86"이다. Both두 are별 [[chemically모두 peculiar star|emically화학적으로 peculiar특이한 star]]s;별로<ref name="skiff">{{cite journal|last1=Skiff|first1=B. A.|year=2014|title=VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)|journal=VizieR On-line Data Catalog|bibcode=2014yCat....1.2023S}}</ref> both둘 are다 catalogued as [[Ap star]]s,별로 although등재되어 component있다. F다만 is종종 sometimesF를 thoughtAm to별로 be an [[Am분류하기도 star]]한다.<ref name=abt/>
 
The [[Washington Double Star Catalog]] lists two fainter companions, C and D, at 47" and 64" separation, respectively.<ref name="wds">{{cite journal|bibcode=2001AJ....122.3466M|title=The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog|journal=The Astronomical Journal|volume=122|issue=6|pages=3466|last1=Mason|first1=Brian D.|last2=Wycoff|first2=Gary L.|last3=Hartkopf|first3=William I.|last4=Douglass|first4=Geoffrey G.|last5=Worley|first5=Charles E.|year=2001|doi=10.1086/323920|doi-access=free}}</ref> Component C has been observed to vary in brightness by over a magnitude, but the type of variability is not known.<ref name="proust">{{cite journal|last1=Proust|first1=D.|last2=Ochsenbein|first2=F.|last3=Pettersen|first3=B. R.|year=1981|title=A catalogue of variable-visual binary stars|journal=Astronomy and Astrophysics Supplement Series|volume=44|pages=179|bibcode=1981A&AS...44..179P}}</ref>
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