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盾牌座γ

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盾牌座γ(γ Scuti)
盾牌座γ的位置(红圈)
观测资料
历元 J2000
星座 盾牌座
星官
赤经 18h 29m 11.85388s[1]
赤纬 -14° 33′ 56.9319″[1]
视星等(V) 4.67[2]
特性
光谱分类A2:V[3]
U−B 色指数+0.04[4]
B−V 色指数+0.07[4]
天体测定
径向速度 (Rv)-41.00[5] km/s
自行 (μ) 赤经:+3.22[1] mas/yr
赤纬:−4.02[1] mas/yr
视差 (π)10.21 ± 0.24[1] mas
距离319 ± 8 ly
(98 ± 2 pc)
绝对星等 (MV)−0.28[2]
详细资料
质量2.91[6] M
半径4.1[7] R
表面重力 (log g)2.09[8]
亮度150[6] L
温度9,016[6] K
自转速度 (v sin i)222[6] km/s
年龄237[8] Myr
其他命名
γ Sct、​BD−14° 5071、​FK5 696、​GC 25220、​HD 170296、​HIP 90595、​HR 6930、​SAO 161520、​GSC 05702-02882
参考资料库
SIMBAD资料

盾牌座γ,名称来自拉丁文的Gamma Scuti,是一颗单独的[9],白色的恒星,位置在盾牌座的南部。它的视星等为4.67[2],表明这虽然是一颗暗星,但在足够黑暗的场所依然可以肉眼看见。根据从地球上观察到的10.21mas的周年视差[1],这颗恒星距离太阳约319光年。现时,它正以41km/s的速度向太阳系移动,这意味著在235万年后,它将以 20 ly(5.519 pc)的距离掠过[10],可能有一段时间成为夜空中最亮的恒星:视星等 − 2.1等[11]

这是一颗A型主序星[3]恒星分类为A2V[3],年龄约2亿3,700万年[8]。它以222km/s的投影旋转速度快速旋转[6]。这使恒星形成略为扁平的形状,具有显著的赤道隆起,估计比极半径大21%[12]。估计这颗恒星的质量是太阳的2.91倍[6],半径是太阳的4.1倍[7]。在表面9,016K的有效温度下,来自其光球的辐射是太阳光度的150倍[6]

参考资料

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  4. ^ 4.0 4.1 Mallama, A. Sloan Magnitudes for the Brightest Stars. The Journal of the American Association of Variable Star Observers. 2014, 42 (2): 443. Bibcode:2014JAVSO..42..443M. Vizier catalog entry页面存档备份,存于互联网档案馆
  5. ^ Gontcharov, G. A. Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system. Astronomy Letters. 2006, 32 (11): 759–771. Bibcode:2006AstL...32..759G. S2CID 119231169. arXiv:1606.08053可免费查阅. doi:10.1134/S1063773706110065. 
  6. ^ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Zorec, J.; Royer, F. Rotational velocities of A-type stars. Astronomy & Astrophysics. 2012, 537: A120. Bibcode:2012A&A...537A.120Z. S2CID 55586789. arXiv:1201.2052可免费查阅. doi:10.1051/0004-6361/201117691.  Vizier catalog entry页面存档备份,存于互联网档案馆
  7. ^ 7.0 7.1 Allende Prieto, C.; Lambert, D. L. Fundamental parameters of nearby stars from the comparison with evolutionary calculations: Masses, radii and effective temperatures. Astronomy and Astrophysics. 1999, 352: 555–562. Bibcode:1999A&A...352..555A. arXiv:astro-ph/9911002可免费查阅.  Vizier catalog entry页面存档备份,存于互联网档案馆
  8. ^ 8.0 8.1 8.2 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可免费查阅. doi:10.1088/0004-637X/804/2/146.  Vizier catalog entry页面存档备份,存于互联网档案馆
  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可免费查阅, 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可免费查阅, doi:10.1051/0004-6361/201425221, A35. 
  11. ^ Kaler, Jim. Gamma Scuti. [2017-04-21]. (原始内容存档于2016-03-05). 
  12. ^ van Belle, Gerard T., Interferometric observations of rapidly rotating stars, The Astronomy and Astrophysics Review, March 2012, 20 (1): 51, Bibcode:2012A&ARv..20...51V, S2CID 119273474, arXiv:1204.2572可免费查阅, doi:10.1007/s00159-012-0051-2.