사용자:Ta183ta/연습장: 두 판 사이의 차이

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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.<ref name=carrier>{{cite journal|doi=10.1051/0004-6361:20020174 |title=Search for duplicity in periodic variable Be stars |journal=Astronomy and Astrophysics |volume=385 |issue=2 |pages=488 |year=2002 |last1=Carrier |first1=F. |last2=Burki |first2=G. |last3=Burnet |first3=M. |bibcode = 2002A&A...385..488C |doi-access=free }}</ref>
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.<ref name=carrier>{{cite journal|doi=10.1051/0004-6361:20020174 |title=Search for duplicity in periodic variable Be stars |journal=Astronomy and Astrophysics |volume=385 |issue=2 |pages=488 |year=2002 |last1=Carrier |first1=F. |last2=Burki |first2=G. |last3=Burnet |first3=M. |bibcode = 2002A&A...385..488C |doi-access=free }}</ref>


==Companions==
==동반 천체==
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,<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" />
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,<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" />


115번째 줄: 115번째 줄:
{| class="wikitable plainrowheaders sortable"
{| class="wikitable plainrowheaders sortable"
|-
|-
! scope="col" style="width:30px;" rowspan=2 | Component<ref>{{cite simbad|title=ADS 11745}}</ref>
! scope="col" style="width:30px;" rowspan=2 | 구성원<ref>{{cite simbad|title=ADS 11745}}</ref>
! scope="col" style="width:70px;" rowspan=2 | Spectral Class
! scope="col" style="width:70px;" rowspan=2 | 분광형
! scope="col" style="width:110px;" rowspan=2 | Magnitude (G)
! scope="col" style="width:110px;" rowspan=2 | 겉보기등급 (G)
! scope="col" style="width:330px;" colspan=2 | Proper Motion
! scope="col" style="width:330px;" colspan=2 | 고유운동
! scope="col" style="width:150px;" rowspan=2 | Radial Velocity (km/s)
! scope="col" style="width:150px;" rowspan=2 | 시선속도 (km/s)
! scope="col" style="width:150px;" rowspan=2 | Parallax (mas)
! scope="col" style="width:150px;" rowspan=2 | 연주시차 (mas)
! scope="col" style="width:50px;" rowspan=2 | Simbad
! scope="col" style="width:50px;" rowspan=2 | Simbad
|-
|-
! scope="col" style="width:150px;" |RA (mas/yr)
! scope="col" style="width:150px;" |적경 (mas/yr)
! scope="col" style="width:180px;" |δ (mas/yr)
! scope="col" style="width:180px;" |적위 (mas/yr)
|-
|-
! scope="row" | A<ref>{{cite DR2|2090687795054381056}}</ref>
! scope="row" | A<ref>{{cite DR2|2090687795054381056}}</ref>
182번째 줄: 182번째 줄:
{{notelist}}
{{notelist}}


== See also ==
== 각주 ==
* [[Stars and planetary systems in fiction#Sheliak (Beta Lyrae)|Beta Lyrae in fiction]]

==Notes==
{{Reflist|30em|refs=
{{Reflist|30em|refs=


2020년 9월 8일 (화) 05:03 판

거문고자리 베타
거문고자리 베타의 위치(붉은 원)
거문고자리 베타의 위치(붉은 원)
관측 정보
(역기점 J2000.0)
별자리 거문고자리
적경(α) 18h 50m 04.79525s[1]
적위(δ) +33° 21′ 45.6100″[1]
겉보기등급(m) 3.52[2] (3.25 – 4.36[3])
성질
분광형 B6-8II[4][5] + B[2] + ? + B7V + ? + B2 + K3V + G5 + G5
U-B 색지수 −0.56[6]
B-V 색지수 +0.00[6]
항성 목록

겉보기등급순 · 절대등급순
거리순 · 질량순 · 반지름순

틀:Starbox astrometry 틀:Starbox orbit 틀:Starbox detail 틀:Starbox catalog 틀:Starbox reference |}

거문고자리 베타(β Lyrae, β Lyr)는 거문고자리 방향에 있는 다중성계이다. 히파르코스 임무 중 얻은 시차 수치에 따르면 베타별은 태양으로부터 약 960 광년 (290 파섹) 떨어져 있다.

이 별은 맨눈에 광점 하나처럼 보이나 실제로는 겉보기 등급 14.3 이상의 항성 여섯 개로 이루어져 있다. 거문고자리 베타 A 명칭을 받은 가장 밝은 구성원은 그 자체가 다시 삼중성계로 식쌍성계 Aa와 단독성 Ab로 구성되어 있다. 식쌍성계 Aa의 구성원 둘은 거문고자리 베타 Aa1 (항성계의 전통적 명칭 셸리아크 Sheliak 를 공식 명칭으로 부여받았음)과[7] Aa2이다. 계의 나머지 구성원 다섯(거문고자리 베타 B, C, D, E, F)은 현 시점에서 모두 단독성으로 추정된다.[8][9][10][11][12][13]

명명법

거문고자리 베타(β Lyrae)는 이 항성계를 바이어 명명법(요한 바이어가 1603년 우라노메트리아에서 창안)으로 표기한 명칭이다. WDS J18501+3322는 워싱턴 이중성 목록에 등재된 명칭이다. The designations of the constituents as Beta Lyrae A, B and C, or alternatively WDS J18501+3322A, B and C, and additionally WDS J18501+3322D, E and F, and those of A's components - Beta Lyrae Aa, Aa1, Aa2 and Ab - derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[14]

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.[15] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[16] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[17] 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.[7]

In Chinese astronomy, Tsan Tae (漸台 (Jiāntāi), meaning Clepsydra Terrace, refers to an asterism consisting of this star, Delta² Lyrae, Gamma Lyrae and Iota Lyrae.[18] Consequently, the Chinese name for Beta Lyrae itself is 漸台二 (Jiāntāièr, 영어: the Second Star of Clepsydra Terrace.)

특징

Beta Lyrae resolved using the CHARA array

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]

Variability

The variable luminosity of this system was discovered in 1784 by the British amateur astronomer John Goodricke.[19] 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[20] and the Michigan InfraRed Combiner (MIRC)[21] 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.[22]

동반 천체

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,[23] but the 2004 release of the SB9 catalog of Spectroscopic Binary Orbits omitted it, so it is now considered a single star.[9]

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 stars;[24] both are catalogued as Ap stars, although component F is sometimes thought to be an Am star.[25]

The Washington Double Star Catalog lists two fainter companions, C and D, at 47" and 64" separation, respectively.[26] Component C has been observed to vary in brightness by over a magnitude, but the type of variability is not known.[27]

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.[25] 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 3.4 mas.[4]

The Gaia spacecraft has provided these data for the stars listed in the WDS:

구성원[28] 분광형 겉보기등급 (G) 고유운동 시선속도 (km/s) 연주시차 (mas) Simbad
적경 (mas/yr) 적위 (mas/yr)
A[29] B7Ve[a] 3.25 – 4.36 1.569 ± 0.582 -2.523 ± 0.594 2.20 ± 0.7 1.0851 ± 0.3398 [8]
B[30] B7V 7.19 4.373 ± 0.087 -0.982 ± 0.098 -14 ± 5 3.0065 ± 0.0542 [9]
C[31] B2 13.07 -1.936 ± 0.024 -1.824 ± 0.030 ? 0.2384 ± 0.0151 [10]
D[32] K3V 14.96 -0.108 ± 0.062 -17.792 ± 0.074 ? 0.8378 ± 0.0368 [11]
E[33] G5 9.77 1.649 ± 0.051 0.719 ± 0.053 1.4 1.6209 ± 0.0339 [12]
F[34] G5 10.10 1.258 ± 0.047 -3.793 ± 0.052 -16.83 ± 1.41 3.5222 ± 0.0307 [13]
  1. ↑ Gaia DR2 astrometric quality considered to be "terrible" for β Lyr A[4]

각주

  1. ↑ 가 나 van Leeuwen, F. (November 2007), “Validation of the new Hipparcos reduction”, 《Astronomy and Astrophysics》 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ↑ 가 나 다 라 마 Zhao, M.; 외. (September 2008), “First Resolved Images of the Eclipsing and Interacting Binary β Lyrae”, 《The Astrophysical Journal》 684 (2): L95–L98, arXiv:0808.0932, Bibcode:2008ApJ...684L..95Z, doi:10.1086/592146. 
  3. ↑ 가 나 인용 오류: <ref> 태그가 잘못되었습니다; gcvs라는 이름을 가진 주석에 텍스트가 없습니다
  4. ↑ 가 나 다 Bastian, U. (2019). “Gaia 8: Discovery of a star cluster containing β Lyrae”. 《Astronomy & Astrophysics》 630: L8. Bibcode:2019A&A...630L...8B. doi:10.1051/0004-6361/201936595. 
  5. ↑ Mourard, D.; Brož, M.; Nemravová, J. A.; Harmanec, P.; Budaj, J.; Baron, F.; Monnier, J. D.; Schaefer, G. H.; Schmitt, H.; Tallon-Bosc, I.; Armstrong, J. T.; Baines, E. K.; Bonneau, D.; Božić, H.; Clausse, J. M.; Farrington, C.; Gies, D.; Juryšek, J.; Korčáková, D.; McAlister, H.; Meilland, A.; Nardetto, N.; Svoboda, P.; Šlechta, M.; Wolf, M.; Zasche, P. (2018). “Physical properties of β Lyrae a and its opaque accretion disk”. 《Astronomy and Astrophysics》 618: A112. arXiv:1807.04789. Bibcode:2018A&A...618A.112M. doi:10.1051/0004-6361/201832952. 
  6. ↑ 가 나 Nicolet, B. (1978), “Photoelectric photometric Catalogue of homogeneous measurements in the UBV System”, 《Observatory》, Bibcode:1978ppch.book.....N. 
  7. ↑ 가 나 “Naming Stars”. IAU.org. 2018년 6월 18일에 확인함. 
  8. ↑ 가 나 “bet Lyr -- Eclipsing binary of beta Lyr type”, 《SIMBAD》 (Centre de Données astronomiques de Strasbourg), 2018년 7월 6일에 확인함. 
  9. ↑ 가 나 다 “bet Lyr B -- Star”, 《SIMBAD》 (Centre de Données astronomiques de Strasbourg), 2018년 7월 6일에 확인함. 
  10. ↑ 가 나 “bet Lyr C -- Star”, 《SIMBAD》 (Centre de Données astronomiques de Strasbourg), 2018년 7월 6일에 확인함. 
  11. ↑ 가 나 “UCAC3 247-141831 -- Star”, 《SIMBAD》 (Centre de Données astronomiques de Strasbourg), 2018년 7월 6일에 확인함. 
  12. ↑ 가 나 “BD+33 3222 -- Star”, 《SIMBAD》 (Centre de Données astronomiques de Strasbourg), 2018년 7월 6일에 확인함. 
  13. ↑ 가 나 “BD+33 3225 -- Star”, 《SIMBAD》 (Centre de Données astronomiques de Strasbourg), 2018년 7월 6일에 확인함. 
  14. ↑ 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]. 
  15. ↑ Allen, Richard Hinckley (1899), “Star-names and their meanings”, 《New York》: 287, Bibcode:1899sntm.book.....A. 
  16. ↑ 《IAU Working Group on Star Names (WGSN)》, International Astronomical Union, 2016년 5월 22일에 확인함. 
  17. ↑ “WG Triennial Report (2015-2018) - Star Names” (PDF). 5쪽. 2018년 7월 14일에 확인함. 
  18. ↑ (중국어) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 3 日
  19. ↑ Hoskin, M. (1979), “Goodricke, Pigott and the Quest for Variable Stars”, 《Journal for the History of Astronomy》 10: 23–41, Bibcode:1979JHA....10...23H, doi:10.1177/002182867901000103. 
  20. ↑ ten Brummelaar, Theo; 외. (July 2005), “First Results from the CHARA Array. II. A Description of the Instrument”, 《The Astrophysical Journal》 628 (453): 453–465, arXiv:astro-ph/0504082, Bibcode:2005ApJ...628..453T, doi:10.1086/430729. 
  21. ↑ Monnier, John D.; 외. (2006), “Michigan Infrared Combiner (MIRC): commissioning results at the CHARA Array” (PDF), 《Proceedings of the SPIE》, Advances in Stellar Interferometry 6268 (62681P): 62681P, Bibcode:2006SPIE.6268E..1PM, doi:10.1117/12.671982. 
  22. ↑ Carrier, F.; Burki, G.; Burnet, M. (2002). “Search for duplicity in periodic variable Be stars”. 《Astronomy and Astrophysics》 385 (2): 488. Bibcode:2002A&A...385..488C. doi:10.1051/0004-6361:20020174. 
  23. ↑ Abt, Helmut A.; Jeffers, Hamilton M.; Gibson, James; Sandage, Allan R. (1961년 9월 20일). “The Visual Multiple System Containing Beta Lyrae”. 《The Astrophysical Journal》 135: 429. Bibcode:1962ApJ...135..429A. doi:10.1086/147282. 
  24. ↑ 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. 
  25. ↑ 가 나 Abt, H. A.; Levy, S. G. (1976). “Visual multiples. III. ADS 11745 (beta Lyrae group)”. 《The Astronomical Journal》 81: 659. Bibcode:1976AJ.....81..659A. doi:10.1086/111936. 
  26. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). “The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog”. 《The Astronomical Journal》 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920. 
  27. ↑ 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. 
  28. ↑ “ADS 11745”. 《SIMBAD》. Centre de données astronomiques de Strasbourg. 
  29. ↑ Brown, A. G. A.; 외. (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.  이 출처의 Gaia DR2 기록 - VizieR.
  30. ↑ Brown, A. G. A.; 외. (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.  이 출처의 Gaia DR2 기록 - VizieR.
  31. ↑ Brown, A. G. A.; 외. (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.  이 출처의 Gaia DR2 기록 - VizieR.
  32. ↑ Brown, A. G. A.; 외. (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.  이 출처의 Gaia DR2 기록 - VizieR.
  33. ↑ Brown, A. G. A.; 외. (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.  이 출처의 Gaia DR2 기록 - VizieR.
  34. ↑ Brown, A. G. A.; 외. (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.  이 출처의 Gaia DR2 기록 - VizieR.

인용 오류: <references> 안에 정의된 "Anderson2012"이라는 이름을 가진 <ref> 태그가 위에서 사용되고 있지 않습니다.
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External links

틀:Stars of Lyra

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