参旗六
 | |
| 观测资料 历元 J2000.0 | |
|---|---|
| 星座 | 猎户座 |
| 星官 | 毕宿 参旗 |
| 赤经 | 04h 49m 50.41091s[1] |
| 赤纬 | +06° 57′ 40.5883″[1] |
| 视星等（V） | 3.16[2] |
| 特性 | |
| 光谱分类 | F6 V[2] |
| U−B 色指数 | +0.00[2] |
| B−V 色指数 | +0.46[2] |
| 变星类型 | 疑似变星[3] |
| 天体测定 | |
| 径向速度 (Rv) | 24.1[4] km/s |
| 自行 (μ) | 赤经：464.06[1] mas/yr 赤纬：11.21[1] mas/yr |
| 视差 (π) | 123.94 ± 0.17[1] mas |
| 距离 | 26.32 ± 0.04 ly (8.07 ± 0.01 pc) |
| 绝对星等 (MV) | 3.65[5] |
| 详细资料 | |
| 质量 | 1.236[6] M☉ |
| 半径 | 1.323 ± 0.004[7] R☉ |
| 表面重力 (log g) | 4.4[8] |
| 亮度 | 2.822 ± 0.030[7] L☉ |
| 温度 | 6,516 ± 19[7] K |
| 金属量 [Fe/H] | 0.02[8] dex |
| 自转速度 (v sin i) | 17[9] km/s |
| 年龄 | 1.4[5] Gyr |
| 其他命名 | |
参旗六，即猎户座π3（Pi3 Orionis、π3 Ori、π3 Orionis），是一颗位于猎户座的恒星，西方传统名称是 Tabit[11]，佛兰斯蒂德命名法将该恒星命名为猎户座1（1 Orionis）。它的视星等是肉眼可见的3.16[2]。参旗六是猎户座中代表狮皮（或盾牌）的恒星中最亮的。根据视差量测，它和地球的距离是26.32光年（8.07秒差距）[1]。虽然在参旗六旁至今并未发现太阳系外行星，该恒星仍被部分天文学家[谁？]认为它周围的特定位置允许体积和地球相当的行星存在。
物理性质
参旗六是一颗光谱类型 F6 V 的主序星，自1943年起它的光谱就是该型恒星的标准光谱[12]。它的质量是太阳的124%[6]，半径比太阳大32%，并且光度几乎是太阳的3倍[7]。它的外层气体有效温度是6,516 K[7]，因此属于黄白色的F-型主序星。参旗六很可能是单一恒星，天球上与它接近的另一颗恒星是光学双星[13]。
虽然参旗六的径向速度会以73.26日的周期变化，引起变化的原因较可能是恒星本身的活动，而非距离它相当近的行星引起。目前并未侦测到参旗六周围有次恒星伴星存在，而麦克唐纳天文台的一个团队则认为在质量0.84到46.7倍木星质量，距离母恒星0.05到5.2天文单位的限制条件下会有一或多颗行星存在[14]。此外，到目前为止即使有类似地球的行星存在，也并未观测到其重力对母恒星运动造成扰动。
参见
- 猎户座π
参考资料
- ^ 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, arXiv:0708.1752
, doi:10.1051/0004-6361:20078357.
- ^ 2.0 2.1 2.2 2.3 2.4 Johnson, H. L.; Morgan, W. W., Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas, Astrophysical Journal, 1953, 117: 313–352, Bibcode:1953ApJ...117..313J, doi:10.1086/145697.
- ^ Kukarkin, B. V.; et al., Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars), Moscow: Academy of Sciences USSR Shternberg, 1981, Bibcode:1981NVS...C......0K.
- ^ Evans, D. S., The Revision of the General Catalogue of Radial Velocities, Batten, Alan Henry; Heard, John Frederick (编), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, June 20–24, 1966, Bibcode:1967IAUS...30...57E.
- ^ 5.0 5.1 Holmberg, J.; Nordström, B.; Andersen, J., The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics, Astronomy and Astrophysics, Supplement Series, July 2009, 501 (3): 941−947, Bibcode:2009A&A...501..941H, arXiv:0811.3982 , doi:10.1051/0004-6361/200811191. Note: see VizieR catalogue V/130 （页面存档备份，存于互联网档案馆）.
- ^ 6.0 6.1 Takeda, G.; et al., Stellar parameters of nearby cool stars. II. Physical properties of ~1000 cool stars from the SPOCS catalog, Astrophysical Journal Supplement Series, 2007, 168: 297–318, Bibcode:2008yCat..21680297T Note: see VizieR catalogue J/ApJS/168/297 （页面存档备份，存于互联网档案馆）.
- ^ 7.0 7.1 7.2 7.3 7.4 Boyajian, Tabetha S.; et al, Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars, The Astrophysical Journal, February 2012, 746 (1): 101, Bibcode:2012ApJ...746..101B, arXiv:1112.3316 , doi:10.1088/0004-637X/746/1/101. See Table 10.
- ^ 8.0 8.1 Kuroczkin, D.; Wiszniewski, A., The problem of iron abundance in the SMR stars., Acta Astronomica, 1997, 27: 145–150, Bibcode:1977AcA....27..145K.
- ^ Bernacca, P. L.; Perinotto, M., A catalogue of stellar rotational velocities, Contributi Osservatorio Astronomico di Padova in Asiago, 1970, 239 (1), Bibcode:1970CoAsi.239....1B.
- ^ 1 Ori -- Variable Star, SIMBAD Astronomical Object Database (Centre de Données astronomiques de Strasbourg), [2011-01-07], （原始内容存档于2016-03-12）
- ^ Moore, Patrick; Rees, Robin, Patrick Moore's Data Book of Astronomy 2nd, Cambridge University Press: 460, 2011 [2012-10-15], ISBN 0521899354, （原始内容存档于2020-09-10）
- ^ 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）
- ^ 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, arXiv:0806.2878 , doi:10.1111/j.1365-2966.2008.13596.x.
- ^ Wittenmyer, Robert A.; et al., Detection Limits from the McDonald Observatory Planet Search Program, The Astronomical Journal, July 2006, 132 (1): 177–188, Bibcode:2006AJ....132..177W, arXiv:astro-ph/0604171 , doi:10.1086/504942.
外部链接
- Pi3 Orionis 2?. SolStation. [2008-07-11]. （原始内容存档于2008-07-19）.
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