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玉井三

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波江座β
Diagram showing star positions and boundaries of the Eridanus constellation and its surroundings
波江座β的位置 (圆圈)
观测资料
历元 J2000.0
星座 波江座
星官 玉井 (参宿)
赤经 05h 07m 50.98549s[1]
赤纬 −05° 05′ 11.2055″[1]
视星等(V) 2.796[2]
特性
光谱分类A3 III var[3]
U−B 色指数+0.124[2]
B−V 色指数+0.110[2]
R−I 色指数+0.08[4]
天体测定
径向速度 (Rv)–3.6[5] km/s
自行 (μ) 赤经:-82.82[1] mas/yr
赤纬:-75.39[1] mas/yr
视差 (π)36.50 ± 0.42[1] mas
距离89 ± 1 ly
(27.4 ± 0.3 pc)
详细资料
质量2.6[6] M
半径3.55[6] R
表面重力 (log g)3.58[5]
亮度52[6] L
温度8,104[5] K
金属量 [Fe/H]–0.4[7] dex
自转速度 (v sin i)196[3] km/s
其他命名
Cursa, Dhalim,[8] Kursa,[9] β Eri, Beta Eridani, Beta Eri, 67 Eridani, 67 Eri, BD−05 1162, CCDM J05079-0506A, FK5 188, GC 6274, GJ 9175, HD 33111, HIP 23875, HR 1666, IDS 05030-0513 A, PPM 187729, SAO 131794, WDS 05078-0505A.[10]
参考数据库
SIMBAD资料

玉井三 (波江座β) 是波江座的第二亮星,位于这个星座东北方的边界,靠近猎户座之处。它的固有名称是Cursa[4][11]视星等2.796[2],所以用肉眼就可以直接看见。视差测量出这颗恒星与地球的距离大约是89光年(27秒差距[1]

性质

玉井三 (波江座β)的光谱类型是A3 III [3],其中的III指出在光度分类中是已经耗尽核心的氢,离开主序带巨星。 外层的有效温度大约是8,104K[5],因此是颗白色色调的A型恒星[12]。这颗投影自转速度高达196 km s–1[3],相较于太阳赤道2 km s–1,是非常的快速[13]。这颗恒星的视星等在2.72-2.80[14] 据报尤其于1985年曾有强劲爆发[11][15]

这颗星的位置和移动轨迹显示它是大熊座星群的成员,一个恒星的集团,它们在空间中有着共同的来源和移动方向。但是,它在光度测量上的属性显示他可能只是个闯入者[5]。玉井三有一颗视星等10.90等的光学伴星角距离为120弧秒方位角 148°[16],在CCDMJ目录上的编号为 CCDM J05079-0506B.[17]

语源

Cursa衍生于Al Kursiyy al Jauzah,意思是"中央的椅子 (或"脚凳") "。这个名称之下的恒星组合还包括玉井一玉井二玉井四[8]

中国,这颗恒星称为玉井三,也就是星官玉井的第三颗星。这个小星群还包括玉井一 (波江座λ)、玉井四 (猎户座τ)和玉井二 (波江座ψ)[18]。当然,玉井三 (波江座β)也包含在内[8][19]。 依据恒星目录的技术备忘录33-507 – 一份包含537颗恒星的精简目录,Al Kursiyy al Jauzah含有三颗的标题:波江座β是Cursa波江座ψAl Kursiyy al Jauzah I波江座λAl Kursiyy al Jauzah II (排除了猎户座τ)[20]

相关条目

参考文献

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  2. ^ 2.0 2.1 2.2 2.3 Cousins, A. W. J., Standardization of Broadband Photometry of Equatorial Standards, South African Astronomical Observatory Circulars, 1984, 8: 59, Bibcode:1984SAAOC...8...59C 
  3. ^ 3.0 3.1 3.2 3.3 Royer, F.; et al, Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i, Astronomy and Astrophysics, October 2002, 393: 897–911, Bibcode:2002A&A...393..897R, arXiv:astro-ph/0205255可免费查阅, doi:10.1051/0004-6361:20020943 
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  5. ^ 5.0 5.1 5.2 5.3 5.4 King, Jeremy R.; et al, Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group, The Astronomical Journal, April 2003, 125 (4): 1980–2017, Bibcode:2003AJ....125.1980K, doi:10.1086/368241 
  6. ^ 6.0 6.1 6.2 Malagnini, M. L.; Morossi, C., Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars, Astronomy and Astrophysics Supplement Series, November 1990, 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M 
  7. ^ Kamp, I.; Hempel, M.; Holweger, H., Do dusty A stars exhibit accretion signatures in their photospheres?, Astronomy and Astrophysics, June 2002, 388: 978–984, Bibcode:2002A&A...388..978K, arXiv:astro-ph/0204449可免费查阅, doi:10.1051/0004-6361:20020493 
  8. ^ 8.0 8.1 8.2 Allen, R. H., Star Names: Their Lore and Meaning Reprint, New York, NY: Dover Publications Inc: 218, 1963 [2010-12-12], ISBN 0-486-21079-0, (原始内容存档于2023-07-01) 
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  11. ^ 11.0 11.1 Kaler, James B., Cursa (Beta Eridani), Stars (University of Illinois), [2012-01-10], (原始内容存档于2012-05-02) 
  12. ^ The Colour of Stars, Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004 [2012-01-16], (原始内容存档于2012-03-10) 
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