玉井三 (波江座β) 是波江座的第二亮星,位於這個星座東北方的邊界,靠近獵戶座之處。它的固有名稱是Cursa[4][11]視星等2.796[2],所以用肉眼就可以直接看見。視差測量出這顆恆星與地球的距離大約是89光年(27秒差距[1]

波江座β
Diagram showing star positions and boundaries of the Eridanus constellation and its surroundings
波江座β的位置 (圓圈)
觀測資料
曆元 J2000.0
星座 波江座
星官 玉井 (參宿)
赤經 05h 07m 50.98549s[1]
赤緯 −05° 05′ 11.2055″[1]
視星等(V) 2.796[2]
特性
光譜分類A3 III var[3]
U−B 色指數+0.124[2]
B−V 色指數+0.110[2]
R−I 色指數+0.08[4]
天體測定
徑向速度 (Rv)–3.6[5] km/s
自行 (μ) 赤經:-82.82[1] mas/yr
赤緯:-75.39[1] mas/yr
視差 (π)36.50 ± 0.42[1] mas
距離89 ± 1 ly
(27.4 ± 0.3 pc)
詳細資料
質量2.6[6] M
半徑3.55[6] R
表面重力 (log g)3.58[5]
亮度52[6] L
溫度8,104[5] K
金屬量 [Fe/H]–0.4[7] dex
自轉速度 (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]
參考資料庫
SIMBAD資料

性質

玉井三 (波江座β)的光譜類型是A3 III [3],其中的III指出在光度分類中是已經耗盡核心的氫,離開主序帶巨星。 外層的有效溫度大約是8,104K[5],因此是顆白色色調的A型恆星[12]。這顆投影自轉速度高達196 km s–1[3],相較於太陽赤道2 km s–1,是非常的快速[13]。這顆恆星的視星等在2.72-2.80[14] 據報尤其於1985年曾有強勁爆發[11][15]

這顆星的位置和移動軌跡顯示它是大熊座星群的成員,一個恆星的集團,它們在空間中有著共同的來源和移動方向。但是,它在光度測量上的屬性顯示他可能只是個闖入者[5]。玉井三有一顆視星等10.90等的光學伴星角距離為120弧秒方位角 148°[16],在CCDMJ目錄上的編號為 CCDM J05079-0506B.[17]

語源

Cursa衍生於Al Kursiyy al Jauzah,意思是"中央的椅子 (或"腳凳") "。這個名稱之下的恆星組合還包括玉井一玉井二玉井四[8]

中國,這顆恆星稱為玉井三,也就是星官玉井的第三顆星。這個小星群還包括玉井一 (波江座λ)、玉井四 (獵戶座τ)和玉井二 (波江座ψ)[18]。當然,玉井三 (波江座β)也包含在內[8][19]。 依據恆星目錄的技術備忘錄33-507 – 一份包含537顆恆星的精簡目錄,Al Kursiyy al Jauzah含有三顆的標題:波江座β是Cursa波江座ψAl Kursiyy al Jauzah I波江座λAl Kursiyy al Jauzah II (排除了獵戶座τ)[20]

相關條目

參考文獻

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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 , 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 , 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, (原始內容存檔於2023-07-01) 
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