"사용자:Ta183ta/연습장"의 두 판 사이의 차이

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다음으로 밝은 동반 천체들은 거문고자리 베타 E와 F이다. E의 겉보기 등급은 10.1v, 각거리는 67"이며 F의 겉보기 등급은 10.6v, 각거리는 86"이다. 두 별 모두 화학적으로 특이한 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> 둘 다 [[Ap/Bp 별|Ap 별]]로 등재되어 있다. 다만 종종 F를 [[Am 별]]로 분류하기도 한다.<ref name=abt/>
 
The워싱턴 [[Washington이중성 Double목록에는 Star Catalog]]어두운 lists반성 twoC와 fainterD companions,둘이 C수록되어 and있으며 D,이들은 at주성으로부터 각각 47" and, 64"만큼 separation,떨어져 respectively있다.<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> Component구성원 CC는 has밝기가 been observed to vary in brightness by over a magnitude,1 but등급을 the넘게 type변화해 of왔으나 variability변광의 is유형은 not밝혀지지 known않았다.<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>
 
Components구성원 A, B, and F 셋은 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.<ref name="abt">{{cite journal|bibcode=1976AJ.....81..659A|title=Visual multiples. III. ADS 11745 (beta Lyrae group)|journal=The Astronomical Journal|volume=81|pages=659|last1=Abt|first1=H. A.|last2=Levy|first2=S. G.|year=1976|doi=10.1086/111936}}</ref> Analysis of [[Gaia 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 all [[main 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 is {{val|3.4|ul=mas}}.<ref name="bastian2019" />
 
The [[Gaia (spacecraft)|Gaia spacecraft]] has provided these data for the stars listed in the WDS: