轩辕十一

轩辕十一,即狮子座ζZeta Leonis、ζ Leo、ζ Leonis),是狮子座一颗视星等3等的恒星。它的西方固有名称 Adhafera(或 Aldhafera, Adhafara)是来自阿拉伯语الضفيرةal-ðafīrah),是指狮子的鬃毛。轩辕十一是在轩辕十二之后构成“镰刀”刀锋的第二颗恒星[10]

轩辕十一
Adhafera
ζ Leo
Diagram showing star positions and boundaries of the Leo constellation and its surroundings
红色圆圈中即轩辕十一
观测资料
历元 J2000
星座 狮子座
星官 星宿 轩辕
赤经 10h 16m 41.41597s[1]
赤纬 +23° 25′ 02.3221″[1]
视星等(V) 3.33[2]
特性
光谱分类F0 III[3][4]
U−B 色指数+0.07[2]
B−V 色指数+0.30[2]
变星类型Suspected
天体测定
径向速度 (Rv)-15.6[5] km/s
自行 (μ) 赤经:+18.39[1] mas/yr
赤纬:-6.84[1] mas/yr
视差 (π)11.90 ± 0.18[1] mas
距离274 ± 4 ly
(84 ± 1 pc)
详细资料
质量3[6] M
半径6[7] R
表面重力 (log g)3.0[7]
亮度85[7] L
温度6,792[7] K
金属量 [Fe/H]–0.03[8] dex
自转速度 (v sin i)72.4[7] km/s
其他命名
Adhafera, Aldhafera, Adhafara, ζ Leo, 36 Leo, HR 4031, BD +24°2209, HD 89025, FK5 384, HIP 50335, SAO 81265, GC 14107, NSV 04804, WDS 10167+2325A.[9]
参考数据库
SIMBAD资料

恒星状态

轩辕十一是一颗光谱类型F0 III的巨星。自1943年起它的光谱就成为将其他恒星光谱分类时的标准[4]。它的视星等+3.44,但光度是太阳的85倍[7]。轩辕十一的质量大约是太阳的3倍[6],半径则是太阳的6倍[7]依巴谷卫星量测其视差的结果显示它距离地球大约274光年(84秒差距)[1]

轩辕十一和视星等5.90的狮子座35光学双星。狮子座35在天球上沿着位置角340°处距离轩辕十一325.9角秒[11][12],但两者并非联星系统,狮子座35距离地球只有100光年。

参见

参考资料

  1. ^ 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, doi:10.1051/0004-6361:20078357 
  2. ^ 2.0 2.1 2.2 Fernie, J. D., New UBVRI photometry for 900 supergiants, Astrophysical Journal Supplement Series, May 1983, 52: 7–22, Bibcode:1983ApJS...52....7F, doi:10.1086/190856 
  3. ^ Montes, D.; et al, Late-type members of young stellar kinematic groups - I. Single stars, Monthly Notices of the Royal Astronomical Society, November 2001, 328 (1): 45–63, Bibcode:2001MNRAS.328...45M, arXiv:astro-ph/0106537 , doi:10.1046/j.1365-8711.2001.04781.x 
  4. ^ 4.0 4.1 Garrison, R. F., Anchor Points for the MK System of Spectral Classification, Bulletin of the American Astronomical Society, December 1993, 25: 1319 [2012-02-04], Bibcode:1993AAS...183.1710G, (原始内容存档于2019-06-25) 
  5. ^ Wielen, R.; et al, Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions (35), Astronomisches Rechen-Institut Heidelberg, 1999, Bibcode:1999VeARI..35....1W 
  6. ^ 6.0 6.1 Kaler, James B., ADHAFERA (Zeta Leonis), Stars (University of Illinois), [2010-05-12], (原始内容存档于2016-11-04) 
  7. ^ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 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 
  8. ^ Gray, R. O.; Graham, P. W.; Hoyt, S. R., The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. II. Basic Parameters of Program Stars and the Role of Microturbulence, The Astronomical Journal, April 2001, 121 (4): 2159–2172, Bibcode:2001AJ....121.2159G, doi:10.1086/319957 
  9. ^ zet Leo -- Variable Star, SIMBAD (Centre de Données astronomiques de Strasbourg), [2010-05-12], (原始内容存档于2016-04-02) 
  10. ^ Proctor, Mary, Evenings with the Stars, Popular Astronomy, 1896–7, 4: 565 
  11. ^ CCDM (Catalog of Components of Double & Multiple stars (Dommanget+ 2002), VizieR (Centre de Données astronomiques de Strasbourg), [2010-05-12], (原始内容存档于2020-08-11) 
  12. ^ Adhafera, Alcyone Bright Star Catalogue, [2010-05-12], (原始内容存档于2018-07-02)