厕增五天兔座θ拉丁化的名字来自θLeporis,是一颗孤独的恒星[9]。这颗白色的恒星,位于南天星座天兔座。它的视星等为4.67等[2],使其明亮到可以用肉眼观看。基于从地球量测的每年18.88mas视差[1],该系统位于距离太阳大约173光年之处。这颗恒星大约在160万年前最接近太阳,当时它位于太阳的29光年(9.0秒差距)范围内[10]

厕增五(θ Leporis)
观测资料
历元 J2000.0
星座 天兔座
星官 参宿
赤经 06h 06m 09.32339s[1]
赤纬 −14° 56′ 06.9188″[1]
视星等(V) 4.67[2]
特性
光谱分类A0 V[3]
U−B 色指数+0.00[2]
B−V 色指数+0.05[2]
天体测定
径向速度 (Rv)+32.0[4] km/s
自行 (μ) 赤经:-17.61[1] mas/yr
赤纬:+12.79[1] mas/yr
视差 (π)18.88 ± 0.54[1] mas
距离173 ± 5 ly
(53 ± 2 pc)
绝对星等 (MV)+1.05[5]
详细资料
质量2.35±0.03[6] M
表面重力 (log g)4.12[7]
亮度41[6] L
温度10,453±355[7] K
自转速度 (v sin i)246[7] km/s
年龄207[7] Myr
其他命名
θ Lep、​18 Lep、​BD−14° 1331、​FK5 2466、​GC 7742、​HD 41695、​HIP 28910、​HR 2155、​SAO 151110[8]
参考资料库
SIMBAD资料

这是一颗普通的A型主序星恒星分类为A0V[3], 年龄约2.07亿年[7]。它以207公里/秒的投影自转速度快速旋转[7]。这使这颗恒星具有扁球的形状,估计赤道隆起比极半径大10%[11]。估计它的质量为2.35太阳质量[6],来自光球的光度是太阳光度的41倍[6],表面的有效温度为10,453k[7]

参考资料

编辑
  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, 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 Johnson, H. L.; et al, UBVRIJKL photometry of the bright stars, Communications of the Lunar and Planetary Laboratory, 1966, 4 (99): 99, Bibcode:1966CoLPL...4...99J. 
  3. ^ 3.0 3.1 Houk, N., Michigan catalogue of two-dimensional spectral types for the HD stars 4, Ann Arbor: Dept. of Astronomy, University of Michigan, 1988, Bibcode:1988mcts.book.....H. 
  4. ^ Gontcharov, G. A., Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system, Astronomy Letters, November 2006, 32 (11): 759–771, Bibcode:2006AstL...32..759G, S2CID 119231169, arXiv:1606.08053 , doi:10.1134/S1063773706110065. 
  5. ^ Anderson, E.; Francis, Ch., XHIP: An extended hipparcos compilation, Astronomy Letters, 2012, 38 (5): 331, Bibcode:2012AstL...38..331A, S2CID 119257644, arXiv:1108.4971 , doi:10.1134/S1063773712050015. 
  6. ^ 6.0 6.1 6.2 6.3 Zorec, J.; Royer, F., Rotational velocities of A-type stars. IV. Evolution of rotational velocities, Astronomy & Astrophysics, January 2012, 537: A120, Bibcode:2012A&A...537A.120Z, S2CID 55586789, arXiv:1201.2052 , doi:10.1051/0004-6361/201117691. 
  7. ^ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 David, Trevor J.; Hillenbrand, Lynne A., The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets, The Astrophysical Journal, 2015, 804 (2): 146, Bibcode:2015ApJ...804..146D, S2CID 33401607, arXiv:1501.03154 , doi:10.1088/0004-637X/804/2/146. 
  8. ^ tet Lep. SIMBAD. 斯特拉斯堡天文资料中心. [2017-08-18]. 
  9. ^ Eggleton, P. P.; Tokovinin, A. A., A catalogue of multiplicity among bright stellar systems, Monthly Notices of the Royal Astronomical Society, September 2008, 389 (2): 869–879, Bibcode:2008MNRAS.389..869E, S2CID 14878976, arXiv:0806.2878 , doi:10.1111/j.1365-2966.2008.13596.x. 
  10. ^ Bailer-Jones, C. A. L., Close encounters of the stellar kind, Astronomy & Astrophysics, March 2015, 575: 13, Bibcode:2015A&A...575A..35B, S2CID 59039482, arXiv:1412.3648 , doi:10.1051/0004-6361/201425221, A35. 
  11. ^ Belle, G. T., Interferometric observations of rapidly rotating stars, The Astronomy and Astrophysics Review, 2012, 20 (1): 51, Bibcode:2012A&ARv..20...51V, S2CID 119273474, arXiv:1204.2572 , doi:10.1007/s00159-012-0051-2.