半人馬座Xi2
半人马座Xi2 （ξ2 Cen, ξ2 Centauri）是在南天半人马座的三星系统[12]，这较宽的光学双星视星等为裸眼可见的+4.30等[2]，略比半人马座ξ1A型主序星暗[13]（+4.83等[14]），年周视差6.98mas，距离太阳大约470光年。在这样的距离，恒星会因为中间的星际尘埃造成消光，而使视星等减弱0.32等[15]
Centaurus constellation map.svg 半人马座ξ2的位置 | |
| 观测资料 历元 J2000.0 | |
|---|---|
| 星座 | 半人马座 |
| 星官 | |
| 赤经 | 13h 06m 54.63940s[1] |
| 赤纬 | −49° 54′ 22.4823″[1] |
| 视星等（V） | 4.30[2] + 9.38[3] |
| 特性 | |
| 光谱分类 | B1.5 V[4] or B2 IV[5] + F7 V[3] |
| U−B 色指数 | −0.810[2] |
| B−V 色指数 | −0.197[2] |
| 天体测定 | |
| 径向速度 (Rv) | +14.3±4.1[6] km/s |
| 自行 (μ) | 赤经：−26.15[1] mas/yr 赤纬：−12.03[1] mas/yr |
| 视差 (π) | 6.98 ± 0.24[1] mas |
| 距离 | 470 ± 20 ly (143 ± 5 pc) |
| 绝对星等 (MV) | −1.51[7] |
| 轨道[8] | |
| 绕行周期 (P) | 7.6497 d |
| 偏心率 (e) | 0.35 |
| 近心点 历元 (T) | 2418077.493 JD |
| 近心点幅角 (ω) (secondary) | 308.6° |
| 半振幅 (K1) (primary) | 38.8 km/s |
| 详细资料 | |
| ξ2 Cen A | |
| 质量 | 8.1±0.1[4] M☉ |
| 表面重力 (log g) | 4.11±0.03[9] |
| 亮度 (bolometric) | 1,702[9] L☉ |
| 温度 | 20,790±335[9] K |
| 自转速度 (v sin i) | 25[10] km/s |
| 年龄 | 11.5±3.7[4] Myr |
| ξ2 Cen B | |
| 质量 | 1.25[9] M☉ |
| 亮度 | 2.4[9] L☉ |
| 温度 | 6,194[9] K |
| 其他命名 | |
| 参考数据库 | |
| SIMBAD | 资料 |
This system was discovered to be a single-lined spectroscopic binary in 1910 by American astronomer Joseph Haines Moore.[16][17] The pair, component A, orbit each other with a period of 7.6497 days and an eccentricity of 0.35.[8] The primary is a B-type star with a stellar classification of B1.5 V[4] or B2 IV,[5] depending on the source. This indicates it may be a main sequence star or a more evolved subgiant star. It has about 8.1[4] times the mass of the Sun and radiates 1,702 times the solar luminosity from its outer atmosphere at an effective temperature of 20,790 K.[9] It is a hybrid pulsator and shows spacings in both g and p modes.[18]
A third star, component B, is a magnitude 9.38 F-type main sequence star with a classification of F7 V. It has 1.25[9] times the mass of the Sun and radiates 2.4[9] times the solar luminosity at an effective temperature of 6,194[9] K. It lies at an angular separation of 25.1 arc seconds from the inner pair.[3] They share a common proper motion, indicating they may be gravitationally bound with an orbital period of around 41,000 years.[19]
The system has a peculiar velocity of 16.2±4.2 km/s.[6] It belongs to the Scorpius–Centaurus association and appears to be a member of the Gould's Belt.[20]
参考
编辑- ^ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F., Validation of the new Hipparcos reduction, Astronomy and Astrophysics, 2007, 474 (2): 653–664, Bibcode:2007A&A...474..653V, S2CID 18759600, arXiv:0708.1752
, doi:10.1051/0004-6361:20078357.
- ^ 2.0 2.1 2.2 2.3 Gutierrez-Moreno, Adelina; Moreno, Hugo, A photometric investigation of the Scorpio-Centaurus association, Astrophysical Journal Supplement, June 1968, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168.
- ^ 3.0 3.1 3.2 Gahm, G. F.; et al, A study of visual double stars with early type primaries. I - Spectroscopic results, Astronomy and Astrophysics Supplement Series, January 1983, 51: 143–159, Bibcode:1983A&AS...51..143G.
- ^ 4.0 4.1 4.2 4.3 4.4 Tetzlaff, N.; et al, A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun, Monthly Notices of the Royal Astronomical Society, January 2011, 410 (1): 190–200, Bibcode:2011MNRAS.410..190T, S2CID 118629873, arXiv:1007.4883 , doi:10.1111/j.1365-2966.2010.17434.x.
- ^ 5.0 5.1 Hohle, M. M.; et al, Masses and luminosities of O- and B-type stars and red supergiants, Astronomische Nachrichten, April 2010, 331 (4): 349, Bibcode:2010AN....331..349H, S2CID 111387483, arXiv:1003.2335 , doi:10.1002/asna.200911355.
- ^ 6.0 6.1 Bobylev, V. V.; Bajkova, A. T., Galactic kinematics from a sample of young massive stars, Astronomy Letters, August 2013, 39 (8): 532–549, Bibcode:2013AstL...39..532B, S2CID 118568203, arXiv:1307.1677 , doi:10.1134/S106377371308001X.
- ^ Anderson, E.; Francis, Ch., XHIP: An extended hipparcos compilation, Astronomy Letters, 2012, 38 (5): 331, Bibcode:2012AstL...38..331A, S2CID 119257644, arXiv:1108.4971 , doi:10.1134/S1063773712050015.
- ^ 8.0 8.1 Pourbaix, D.; et al, SB9: The ninth catalogue of spectroscopic binary orbits, Astronomy & Astrophysics, 2004, 424 (2): 727–732, Bibcode:2004A&A...424..727P, S2CID 119387088, arXiv:astro-ph/0406573 , doi:10.1051/0004-6361:20041213.
- ^ 9.00 9.01 9.02 9.03 9.04 9.05 9.06 9.07 9.08 9.09 Gerbaldi, M.; et al, Binary systems with post-T Tauri secondaries, Astronomy and Astrophysics, November 2001, 379: 162–184, Bibcode:2001A&A...379..162G, doi:10.1051/0004-6361:20011298 .
- ^ Wolff, S. C.; et al, Rotational Velocities for B0-B3 Stars in Seven Young Clusters: Further Study of the Relationship between Rotation Speed and Density in Star-Forming Regions, The Astronomical Journal, 2007, 133 (3): 1092–1103, Bibcode:2007AJ....133.1092W, S2CID 119074863, arXiv:astro-ph/0702133 , doi:10.1086/511002.
- ^ ksi02 Cen -- Spectroscopic binary, SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), [2017-01-09], （原始内容存档于2022-10-31）.
- ^ Eggleton, P. P.; Tokovinin, A. A., A catalogue of multiplicity among bright stellar systems, Monthly Notices of the Royal Astronomical Society, September 2008, 389 (2): 869–879, Bibcode:2008MNRAS.389..869E, S2CID 14878976, arXiv:0806.2878 , doi:10.1111/j.1365-2966.2008.13596.x.
- ^ Backyard Astronomy, The Guides, Fog City Press: 248, 2003, ISBN 1877019321.
- ^ Gutierrez-Moreno, Adelina; Moreno, Hugo, A photometric investigation of the Scorpio-Centaurus association, Astrophysical Journal Supplement, June 1968, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168.
- ^ Gontcharov, G. A., Spatial distribution and kinematics of OB stars, Astronomy Letters, November 2012, 38 (11): 694–706, Bibcode:2012AstL...38..694G, S2CID 119108982, arXiv:1606.09028 , doi:10.1134/S1063773712110035.
- ^ Moore, Joseph Haines, Ten stars having variable radial velocities, Lick Observatory Bulletin, 1910, 6 (182): 55–59, Bibcode:1910LicOB...6...55M, doi:10.5479/ADS/bib/1910LicOB.6.55M.
- ^ Neubauer, F. J., The orbit of the spectroscopic binary ξ2 Centauri, Lick Observatory Bulletin, 1931, 15: 107–108, Bibcode:1931LicOB..15..107N, doi:10.5479/ADS/bib/1931LicOB.15.107N .
- ^ Sharma, Awshesh N.; Bedding, Timothy R.; Saio, Hideyuki; White, Timothy R. Pulsating B stars in the Scorpius–Centaurus Association with TESS. Monthly Notices of the Royal Astronomical Society. 2022, 515: 828–840. Bibcode:2022MNRAS.515..828S. arXiv:2203.02582 . doi:10.1093/mnras/stac1816.
- ^ Tokovinin, A., Comparative statistics and origin of triple and quadruple stars, Monthly Notices of the Royal Astronomical Society, September 2008, 389 (2): 925–938, Bibcode:2008MNRAS.389..925T, S2CID 16452670, arXiv:0806.3263 , doi:10.1111/j.1365-2966.2008.13613.x.
- ^ Bobylev, V. V.; Bajkova, A. T., Kinematics of the Scorpius–Centaurus OB association, Astronomy Letters, September 2007, 33 (9): 571–583, Bibcode:2007AstL...33..571B, S2CID 15785349, arXiv:0708.0943 , doi:10.1134/S1063773707090010.
