弧矢增十七
  | |
| 观测资料 历元 J2000 | |
|---|---|
| 星座 | 船尾座 |
| 星官 | |
| 赤经 | 07h 49m 17.65567s[1] |
| 赤纬 | −24° 51′ 35.2305″[1] |
| 视星等（V） | 3.35[2] |
| 特性 | |
| 光谱分类 | G6 Iab-Ib[3] |
| U−B 色指数 | +1.18[2] |
| B−V 色指数 | +1.25[2] |
| 天体测定 | |
| 径向速度 (Rv) | +2.7[4] km/s |
| 自行 (μ) | 赤经：−4.81[1] mas/yr 赤纬：−0.89[1] mas/yr |
| 视差 (π) | 2.72 ± 0.21[1] mas |
| 距离 | 1,200 ± 90 ly (370 ± 30 pc) |
| 绝对星等 (MV) | –4.73[5] |
| 详细资料 | |
| 质量 | 9.9 ± 1.0[3] M☉ |
| 表面重力 (log g) | 1.21 ± 0.09[3] |
| 亮度 | 60,000[6] L☉ |
| 温度 | 4,880 ± 150[3] K |
| 金属量 [Fe/H] | +0.24[7] dex |
| 自转速度 (v sin i) | 9.2[8] km/s |
| 年龄 | 23[3] Myr |
| 其他命名 | |
| 参考数据库 | |
| SIMBAD | 资料 |
弧矢增十七（Xi Puppis、ξ Puppis，缩写Xi Pup、 ξ Pup）是位于南天星座船尾座的多星系统。它是这个星座中较亮的成员之一，视星等为3.35等[2]。根据在依巴谷任务期间进行的视差测量，它与太阳的距离大约为1,200光年（370秒差距），误差约为7.5%[1]。
该系统由一个光谱联星组成，标示为弧矢增十七A（船尾座Xi A）[9]，与第三颗恒星弧矢增十七B（船尾座Xi B）。弧矢增十七A 的两颗恒星分别标示为弧矢增十七A a（正式命名为"Azmidi"/ˈæzmɪdi/)[10]）和弧矢增十七Ab 。
命名法
[编辑]参考资料
[编辑]- ^ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F., Validation of the new Hipparcos reduction, Astronomy and Astrophysics, November 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 Johnson, H. L.; et al, UBVRIJKL photometry of the bright stars, Communications of the Lunar and Planetary Laboratory, 1966, 4 (99): 99, Bibcode:1966CoLPL...4...99J
- ^ 3.0 3.1 3.2 3.3 3.4 Lyubimkov, Leonid S.; et al, Accurate fundamental parameters for A-, F- and G-type Supergiants in the solar neighbourhood, Monthly Notices of the Royal Astronomical Society, February 2010, 402 (2): 1369–1379, Bibcode:2010MNRAS.402.1369L, S2CID 119096173, arXiv:0911.1335 , doi:10.1111/j.1365-2966.2009.15979.x
- ^ Wilson, R. E. General Catalogue of Stellar Radial Velocities. Carnegie Institute Washington D.C. Publication (Carnegie Institute of Washington D.C.). 1953. Bibcode:1953GCRV..C......0W.
- ^ Luck, R. E., The chemical composition of late-type supergiants. IV - Homogeneous abundances and galactic metallicity trends, Astrophysical Journal, Part 1, 1982-05-01, 256: 177–188, Bibcode:1982ApJ...256..177L, doi:10.1086/159895
- ^ Reimers, D.; Huensch, M.; Schmitt, J. H. M. M.; Toussaint, F. Hybrid stars and the reality of "dividing lines" among G to K bright giants and supergiants. Astronomy and Astrophysics. 1996, 310: 813. Bibcode:1996A&A...310..813R.
- ^ Malagnini, M. L.; Morossi, C.; Buzzoni, A.; Chavez, M. Observations and Atmospheric Parameters of Super-Metal-rich Candidates. The Publications of the Astronomical Society of the Pacific. 2000, 112 (777): 1455. Bibcode:2000PASP..112.1455M. doi:10.1086/317714 .
- ^ De Medeiros, J. R.; Udry, S.; Burki, G.; Mayor, M. A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars. Astronomy and Astrophysics. 2002, 395: 97–98. Bibcode:2002A&A...395...97D. arXiv:1312.3474 . doi:10.1051/0004-6361:20021214.
- ^ Washington Double Star Catalog. United States Naval Observatory. [2018-06-20]. （原始内容存档于2011-02-14）.
- ^ Naming Stars. IAU.org. [2018-06-18]. （原始内容存档于2020-04-11）.
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