"사용자:Ta183ta/연습장"의 두 판 사이의 차이

잔글
편집 요약 없음
잔글
 
==동반 천체==
In거문고자리 addition베타 to외에 Beta동반 Lyrae천체 A,여럿도 several천체목록에 other companions have been catalogued실렸다. β거문고자리 Lyr베타 B,B는 at각거리상으로 an angular separation of주성으로부터 45.7", is떨어져 of있으며 spectral분광형은 typeB7 B7V,V에 has겉보기 an apparent magnitude of등급은 +7.2,2이고 and쌍안경으로 can쉽게 easily be seen있다. withB의 binoculars. It광도는 is태양의 about 80 times as luminous as the Sun배이다. InB는 19621962년 it was identified as spectroscopic binary with a period of공전주기 4.348 days,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 catalog of Spectroscopic Binary Orbits omitted it, so it is now considered a single star.<ref name="SIMBADB" />
 
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 are [[chemically peculiar star|emically peculiar star]]s;<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> both are catalogued as [[Ap star]]s, although component F is sometimes thought to be an [[Am star]].<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>