格利澤673 是一顆位於蛇夫座橙矮星。光譜分類為K7V[2]。這個烘譜類型的主序星質量為太陽質量(M)的60–70%。

Gl 673
觀測資料
曆元 J2000
星座 蛇夫座
星官
赤經 17h 25m 45.23266s[1]
赤緯 +02° 06′ 41.1208″[1]
視星等(V) 7.492[2]
特性
光谱分类K7V[2]
U−B 色指数1.261[2]
B−V 色指数1.373[2]
天体测定
徑向速度 (Rv)−24.4[3] km/s
自行 (μ) 赤经:−579.66[1] mas/yr
赤纬:−1,184.76[1] mas/yr
视差 (π)129.6459 ± 0.0175[4] mas
距离25.157 ± 0.003 ly
(7.713 ± 0.001 pc)
绝对星等 (MV)8.06[2]
詳細資料
半徑0.564[5] R
表面重力 (log g)4.70[6]
溫度4,030[5] K
金属量 [Fe/H]−0.20[6] dex
自轉11.94 days[7]
年齡(205 ± 21) × 106[7]
其他命名
GJ 673, BD +02°3312, HD 157881, LHS 447, LTT 15175, GCTP 3955.00, SAO 122374, Wolf 718, Vys 794, HIP 85295.[8]
參考資料庫
SIMBAD资料
Gliese 673 is located in the constellation Ophiuchus.
Gliese 673 is located in the constellation Ophiuchus.
            Gliese 673
格利澤673在蛇夫座的位置

這顆恆星相對靠近太陽,距離大約25.1光年。然而,儘管如此接近,它仍然太微弱,無法用肉眼觀察到。它被認為是一顆緩慢旋轉的恆星,具有相對較高的自行

格利澤673是附近的橙矮星之一,在類太陽恆星和紅矮星之間的“最佳位置”,就生命存在的可能性及其易探測性而言(在這種情況下,行星可能位於該系統的外部保守宜居帶)。[9]

參見

编辑

參考資料

编辑
  1. ^ 1.0 1.1 1.2 1.3 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. ^ 2.0 2.1 2.2 2.3 2.4 2.5 Koen, C.; et al, UBV(RI)C JHK observations of Hipparcos-selected nearby stars, Monthly Notices of the Royal Astronomical Society, April 2010, 403 (4): 1949–1968, Bibcode:2010MNRAS.403.1949K, doi:10.1111/j.1365-2966.2009.16182.x  
  3. ^ Nordström, B.; et al, The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs, Astronomy and Astrophysics, May 2004, 418: 989–1019, Bibcode:2004A&A...418..989N, S2CID 11027621, arXiv:astro-ph/0405198 , doi:10.1051/0004-6361:20035959 
  4. ^ Brown, A. G. A.; et al. Gaia Early Data Release 3: Summary of the contents and survey properties. Astronomy & Astrophysics. 2021, 649: A1. Bibcode:2021A&A...649A...1G. S2CID 227254300. arXiv:2012.01533 . doi:10.1051/0004-6361/202039657 .  已忽略未知参数|collaboration= (帮助) (勘误: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  5. ^ 5.0 5.1 van Belle, Gerard T.; von Braun, Kaspar, Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars, The Astrophysical Journal, April 2009, 694 (2): 1085–1098, Bibcode:2009ApJ...694.1085V, S2CID 18370219, arXiv:0901.1206 , doi:10.1088/0004-637X/694/2/1085 
  6. ^ 6.0 6.1 Frasca, A.; et al, REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters, Astronomy and Astrophysics, December 2009, 508 (3): 1313–1330, Bibcode:2009A&A...508.1313F, S2CID 118361131, arXiv:0911.0760 , doi:10.1051/0004-6361/200913327 
  7. ^ 7.0 7.1 Barnes, Sydney A., Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors, The Astrophysical Journal, November 2007, 669 (2): 1167–1189, Bibcode:2007ApJ...669.1167B, S2CID 14614725, arXiv:0704.3068 , doi:10.1086/519295 
  8. ^ LHS 447 -- High proper-motion Star, SIMBAD (Centre de Données astronomiques de Strasbourg), [2011-10-15], (原始内容存档于2023-03-28) 
  9. ^ Arney, Giada N. The K Dwarf Advantage for Biosignatures on Directly Imaged Exoplanets. The Astrophysical Journal. 2019, 873 (1): L7. doi:10.3847/2041-8213/ab0651 . 

外部連結

编辑