垒壁阵八
  | |
| 观测资料 历元 J2000 | |
|---|---|
| 星座 | 宝瓶座 |
| 星官 | |
| 赤经 | 23h 14m 19.35965s[1] |
| 赤纬 | –06° 02′ 56.3986″[1] |
| 视星等（V） | +4.223[2] |
| 特性 | |
| 光谱分类 | M1.5 III[3] |
| U−B 色指数 | +1.897[2] |
| B−V 色指数 | +1.563[2] |
| 天体测定 | |
| 径向速度 (Rv) | +2.48±0.32[4] km/s |
| 自行 (μ) | 赤经：+35.391[1] mas/yr 赤纬：–196.862[1] mas/yr |
| 视差 (π) | 14.6670 ± 0.4099[1] mas |
| 距离 | 222 ± 6 ly (68 ± 2 pc) |
| 绝对星等 (MV) | 0.30±0.120[5] |
| 详细资料 | |
| 质量 | 1.00±0.03[6] M☉ |
| 半径 | 34.77+1.83 −2.04[6] R☉ |
| 表面重力 (log g) | 1.5[4] |
| 亮度 | 207.7±25.2[6] L☉ |
| 温度 | 3715±48[6] K |
| 自转速度 (v sin i) | 6.7[4] km/s |
| 年龄 | 10.97±0.83[6] Gyr |
| 其他命名 | |
| 参考数据库 | |
| SIMBAD | 资料 |
垒壁阵八（英语：Phi Aquarii，是源自拉丁化拜耳命名法名称[8]。）是在天球赤道星座宝瓶座中的联星系统。它的综合视星等为+4.223，因此肉眼可见[2]。视差量测表明，它与地球的距离大致为 222光年（68秒差距）[1]，并且它以+2.5km/s的径向速度漂移得更远[4]。它位于黄道以南1.05度，因此受到月掩星的影响，会被月球遮蔽[9]。
它是一个光谱联星的恒星系统，估计周期为2,500天[10]。主星是一颗红巨星，恒星分类为M1.5 III[3]。这颗恒星的质量与太阳相同，但其演化使外层已经膨胀到太阳的35倍大[6]。在3715K的表面有效温度下，它的辐射亮度是太阳的208倍[6]，使其具有M型恒星的红色色调[11]。
参考资料
- ^ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J. H. J.; et al. Gaia Data Release 2. Summary of the contents and survey properties. Astronomy & Astrophysics. 2018. Bibcode:2018A&A...616A...1G. arXiv:1804.09365
. doi:10.1051/0004-6361/201833051. VizieR中此天体在盖亚望远镜第二批数据发布的记录
- ^ 2.0 2.1 2.2 2.3 Gutierrez-Moreno, Adelina; et al, A System of photometric standards, Publications of the Department of Astronomy University of Chile (Publicaciones Universidad de Chile, Department de Astronomy), 1966, 1: 1–17, Bibcode:1966PDAUC...1....1G.
- ^ 3.0 3.1 Morgan, W. W.; Keenan, P. C., Spectral Classification, Annual Review of Astronomy and Astrophysics, 1973, 11: 29, Bibcode:1973ARA&A..11...29M, doi:10.1146/annurev.aa.11.090173.000333.
- ^ 4.0 4.1 4.2 4.3 Massarotti, Alessandro; et al, Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity, The Astronomical Journal, January 2008, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209 .
- ^ Park, Sunkyung; et al, Wilson-Bappu Effect: Extended to Surface Gravity, The Astronomical Journal, 2013, 146 (4): 73, Bibcode:2013AJ....146...73P, S2CID 119187733, arXiv:1307.0592 , doi:10.1088/0004-6256/146/4/73.
- ^ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Baines, Ellyn K.; et al. Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer. The Astronomical Journal. 2018, 155 (1). 30. Bibcode:2018AJ....155...30B. S2CID 119427037. arXiv:1712.08109 . doi:10.3847/1538-3881/aa9d8b .
- ^ * phi Aqr. SIMBAD. 斯特拉斯堡天文资料中心.
- ^ 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.
- ^ White, Nathaniel M.; Feierman, Barry H., A Catalog of Stellar Angular Diameters Measured by Lunar Occultation, Astronomical Journal, September 1987, 94: 751, Bibcode:1987AJ.....94..751W, doi:10.1086/114513.
- ^ Famaey, B.; et al, Spectroscopic binaries among Hipparcos M giants,. I. Data, orbits, and intrinsic variations, Astronomy and Astrophysics, May 2009, 498 (2): 627–640, Bibcode:2009A&A...498..627F, S2CID 18739721, arXiv:0901.0934 , doi:10.1051/0004-6361/200810698.
- ^ The Colour of Stars, Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004 [2012-07-02], （原始内容存档于March 18, 2012）.
