克魯格60Kruger 60)是一個距離地球13.15 光年聯星系統。系統內的兩顆紅矮星以周期44.6年互繞。

克魯格60A/B
Kruger 60 A/B
觀測數據
曆元 J2000      分點
星座 仙王座
Kruger 60 A
赤經 22h 27m 59.4677s[1]
赤緯 +57° 41′ 45.150″[1]
視星等 (V) 9.59
Kruger 60 B
赤經 22h 27m 59.568s[1]
赤緯 +57° 41′ 45.28″[1]
視星等 (V) 11.40
特性
光譜分類M3V/M4V[2]
U−B 色指數1.27/1.3
B−V 色指數1.65/1.8
變星類型無/耀星
天體測定
徑向速度 (Rv)–33.1/–31.9 km/s
自行 (μ) 赤經:–870.23 mas/yr
赤緯:–471.10 mas/yr
視差 (π)248.06 ± 1.39 mas
距離13.15 ± 0.07 ly
(4.03 ± 0.02 pc)
絕對星等 (MV)11.76/13.46
詳細資料
質量0.271/0.176[3] M
半徑0.35/0.24[4] R
亮度0.010/0.0034 L
溫度3180/2890 K K
金屬量–0.04[5]
軌道[6]
主星Kruger 60 A
伴星Kruger 60 B
繞行週期 (P)44.67 yr
半長軸 (a)2.383"
偏心率 (e)0.410
傾斜角 (i)167.2°
升交點黃經 (Ω)154.5°
近心點 曆元 (T)1970.22
近心點幅角 (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]

概述

編輯

系統中較大的稱為克魯格60A,較小的稱為克魯格60B。較大的克魯格60A質量約太陽的27%,半徑則為太陽的35%;較小的克魯格60B其質量約太陽的18%,半徑約太陽的24%[3][4]。克魯格60B是一顆耀星,其變星編號為仙王座DO("DO Cephei").[8]。克魯格60B光度會不規則變化,會在光度加倍後經過8分鐘又恢復原本光度[來源請求]

系統中的兩顆恆星平均距離約9.5天文單位,大約是太陽土星的平均距離。但兩者之間的橢圓形軌道使其距離在5.5到13.5天文單位之間變化[來源請求]

該系統在距離銀河系核心7–9 kpc的距離環繞銀河系中心,軌道離心率約0.126–0.130[9]。該系統將在88,600年後最接近太陽,大約是1.95秒差距[10]

參考資料

編輯
  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 . 
  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 . doi:10.1051/0004-6361:20000451.  The data is from the Vizier II/224頁面存檔備份,存於網際網路檔案館) 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 . 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]. (原始內容存檔於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. 

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