跳转到内容

克鲁格60

维基百科,自由的百科全书
克鲁格60A/B
Kruger 60 A/B
观测数据
历元 J2000      分点
星座 仙王座
Kruger 60 A
赤经 22h 27m 59.4677s[1]
赤纬 +57° 41′ 45.150″[1]
视星等 (V) 9.59
Kruger 60 B
赤经 22h 27m 59.568s[1]
赤纬 +57° 41′ 45.28″[1]
视星等 (V) 11.40
特性
光谱分类M3V/M4V[2]
U−B 色指数1.27/1.3
B−V 色指数1.65/1.8
变星类型无/耀星
天体测定
径向速度 (Rv)–33.1/–31.9 km/s
自行 (μ) 赤经:–870.23 mas/yr
赤纬:–471.10 mas/yr
视差 (π)248.06 ± 1.39 mas
距离13.15 ± 0.07 ly
(4.03 ± 0.02 pc)
绝对星等 (MV)11.76/13.46
详细资料
质量0.271/0.176[3] M
半径0.35/0.24[4] R
亮度0.010/0.0034 L
温度3180/2890 K K
金属量–0.04[5]
轨道[6]
主星Kruger 60 A
伴星Kruger 60 B
绕行周期 (P)44.67 yr
半长轴 (a)2.383"
偏心率 (e)0.410
倾斜角 (i)167.2°
升交点黄经 (Ω)154.5°
近心点 历元 (T)1970.22
近心点幅角 (ω)
(primary)
211.0°
其他命名
DO Cephei, Gl 232-075, GJ 860 A/B, BD +56°2783, HD 239960, LHS 3814/3815, GCTP 5438.00, ADS 15972, Vys 207 A/B, HIP 110893.[7]

克鲁格60Kruger 60)是一个距离地球13.15 光年联星系统。系统内的两颗红矮星以周期44.6年互绕。

概述

系统中较大的称为克鲁格60A,较小的称为克鲁格60B。较大的克鲁格60A质量约太阳的27%,半径则为太阳的35%;较小的克鲁格60B其质量约太阳的18%,半径约太阳的24%[3][4]。克鲁格60B是一颗耀星,其变星编号为仙王座DO("DO Cephei").[8]。克鲁格60B光度会不规则变化,会在光度加倍后经过8分钟又恢复原本光度[来源请求]

系统中的两颗恒星平均距离约9.5天文单位,大约是太阳土星的平均距离。但两者之间的椭圆形轨道使其距离在5.5到13.5天文单位之间变化[来源请求]

该系统在距离银河系核心7–9 kpc的距离环绕银河系中心,轨道离心率约0.126–0.130[9]。该系统将在88,600年后最接近太阳,大约是1.95秒差距[10]

参考资料

  1. ^ 1.0 1.1 1.2 1.3 Perryman, M. A. C.; et al. The Hipparcos Catalogue. Astronomy and Astrophysics. 1997, 323: L49–L52. Bibcode:1997A&A...323L..49P. 
  2. ^ Henry, Todd J.; et al. The solar neighborhood, 1: Standard spectral types (K5-M8) for northern dwarfs within eight parsecs. The Astronomical Journal. October 1994, 108 (4): 1437–1444. Bibcode:1994AJ....108.1437H. doi:10.1086/117167. 
  3. ^ 3.0 3.1 Delfosse, X.; et al. Accurate masses of very low mass stars. IV. Improved mass-luminosity relations. Astronomy and Astrophysics. December 2000, 364: 217–224. Bibcode:2000A&A...364..217D. arXiv:astro-ph/0010586可免费查阅. 
  4. ^ 4.0 4.1 Pasinetti Fracassini, L. E.; et al. Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics. Astronomy and Astrophysics. February 2001, 367 (2): 521–524. Bibcode:2001A&A...367..521P. arXiv:astro-ph/0012289可免费查阅. doi:10.1051/0004-6361:20000451.  The data is from the Vizier II/224页面存档备份,存于互联网档案馆) catalogue.
  5. ^ Bonfils, X.; et al. Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence. Astronomy and Astrophysics. November 2005, 442 (2): 635–642. Bibcode:2005A&A...442..635B. arXiv:astro-ph/0503260可免费查阅. doi:10.1051/0004-6361:20053046.  Only listed for component A.
  6. ^ Heintz, W. D. Orbits of 20 visual binaries. Astronomy and Astrophysics Supplement Series. August 1986, 65 (2): 411–417. Bibcode:1986A&AS...65..411H. 
  7. ^ NSV 14168 – Variable Star. SIMBAD. Centre de Données astronomiques de Strasbourg. [2009-09-28]. (原始内容存档于2020-07-07). 
  8. ^ White, Stephen M.; et al. A VLA survey of nearby flare stars. Astrophysical Journal Supplement Series. December 1989, 71: 895–904. Bibcode:1989ApJS...71..895W. doi:10.1086/191401. 
  9. ^ Allen, C.; Herrera, M. A. The galactic orbits of nearby UV Ceti stars. Revista Mexicana de Astronomia y Astrofisica. 1998, 34: 37–46. Bibcode:1998larm.confE.115A. 
  10. ^ García-Sánchez, J.; et al. Stellar encounters with the solar system. Astronomy and Astrophysics. November 2001, 379 (2): 634–659. Bibcode:2001A&A...379..634G. doi:10.1051/0004-6361:20011330. 

延伸阅读