拉卡伊9352
观测资料 历元 J2000 | |
---|---|
星座 | 南鱼座 |
星官 | |
赤经 | 23h 05m 52.03604s[1] |
赤纬 | −35° 51′ 11.0475″[1] |
视星等(V) | 7.34[2] |
特性 | |
光谱分类 | M0.5V[3] |
U−B 色指数 | +1.18[4] |
B−V 色指数 | +1.50[4] |
变星类型 | 疑似[5] |
天体测定 | |
径向速度 (Rv) | +9.7[6] km/s |
自行 (μ) | 赤经:+6,765.995[7] mas/yr 赤纬:+1,330.388[7] mas/yr |
视差 (π) | 304.1354 ± 0.0200[8] mas |
距离 | 10.7241 ± 0.0007 ly (3.2880 ± 0.0002 pc) |
绝对星等 (MV) | 9.8[9] |
详细资料 | |
质量 | 0.486 ± 0.012[10] M☉ |
半径 | 0.470 ± 0.001[10] R☉ |
表面重力 (log g) | 4.78[10] |
亮度 | ±0.0022 0.0367[10] L☉ |
温度 | ±57 3,692[10] K |
金属量 [Fe/H] | −0.22 ± 0.09[11] dex |
自转速度 (v sin i) | 1[6] km/s |
年龄 | 4.57[12] Gyr |
其他命名 | |
拉卡伊9352(Lac 9352)是位于南天南鱼座的一颗红矮星,视星等为7.34等[4]。这颗恒星太暗,即使在最良好的视相条件下,肉眼也无法观察到。视差量测出它距离地球大约10.74光年(3.29秒差距)[1],是距离太阳系最近的第11个恒星系[13],是星座南鱼座中最接近地球的恒星。ChView模拟[14]显示它最近的邻居是宝瓶座EZ三合星系统,距离它大约4.1光年远。
性质
这颗恒星拥有已知的第四高的自行[15](1881年本杰明·古尔德首次注意到这一点[16]。),每年总共移动6.9弧秒。然而,因为在一个弧度中有3600弧秒,这仍然是一个非常小的整体运动。这颗恒星的空间速度成分是(U, V, W) = (−93.9, −14.1, −51.4) km/s[17]。如果径向速度 ('Vr')等于+9.7公里/秒,那么大约2,700年前拉卡伊9352距离太阳的最近,约为10.63 ly(3.26 pc)[18]。
拉卡伊9352的光谱分类为M0.5V的类型 [3],这表明它是被称为红矮星的主序恒星。这是第一颗量测角直径的红矮星[19],其物理直径约为太阳半径的46%[3]。它大约拥有太阳质量的一半[3],表面的有效温度约为3,626K[3]。
行星系
2020年6月,报告了两颗超级地球行星,以及第三个可能是由于恒星活动造成,周期为50.7天的讯号。然而,如果这真的是颗行星,它可能位于适居带内。它们是用径向速度法从智利HARPS和夏威夷HIRES的观测中检测出来的 [20][21]。
成员 (依恒星距离) |
质量 | 半长轴 (AU) |
轨道周期 (天) |
离心率 | 倾角 | 半径 |
---|---|---|---|---|---|---|
b | ±0.6 ≥ 4.2M⊕ | ±0.002 0.068 | ±0.001 9.262 | +0.09 −0.06 0.09 |
— | — |
c | ±1.2 ≥ 7.6M⊕ | ±0.004 0.120 | +0.004 −0.005 21.789 |
+0.09 −0.10 0.22 |
— | — |
d (未确认) | ≳ 8.3M⊕ | ~0.21 | ~50.7 | +0.20 −0.15 0.25 |
相关条目
参考资料
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- ^ 2.0 2.1 LACAILLE 9352 -- Pre-main sequence Star. SIMBAD. Centre de Données astronomiques de Strasbourg. [2010-01-20]. (原始内容存档于2023-01-28).
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- ^ 7.0 7.1 Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J. H. J.; et al. Gaia Data Release 2. Summary of the contents and survey properties. Astronomy & Astrophysics. 2018. Bibcode:2018A&A...616A...1G. arXiv:1804.09365 . doi:10.1051/0004-6361/201833051. VizieR中此天体在盖亚望远镜第二批数据发布的记录
- ^ Brown, A. G. A.; et al. Gaia Early Data Release 3: Summary of the contents and survey properties. Astronomy & Astrophysics. 2021, 649: A1. Bibcode:2021A&A...649A...1G. S2CID 227254300. arXiv:2012.01533 . doi:10.1051/0004-6361/202039657 . 已忽略未知参数
|collaboration=
(帮助) (勘误: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR. - ^ Murdin, Paul (编). Encyclopedia of Astronomy and Astrophysics. Bristol: Institute of Physics Publishing. November 2000. Bibcode:2000eaa..bookE5158.. ISBN 0333750888. doi:10.1888/0333750888/5158.
absolute magnitude is 9.8
|chapter=
被忽略 (帮助) - ^ 10.0 10.1 10.2 10.3 10.4 Rabus, Markus; Lachaume, Régis; Jordán, Andrés; Brahm, Rafael; Boyajian, Tabetha; Von Braun, Kaspar; Espinoza, Néstor; Berger, Jean-Philippe; Le Bouquin, Jean-Baptiste; Absil, Olivier. A discontinuity in the Teff–radius relation of M-dwarfs. Monthly Notices of the Royal Astronomical Society. 2019, 484 (2): 2674–2683. Bibcode:2019MNRAS.484.2674R. S2CID 119189542. arXiv:1901.08077 . doi:10.1093/mnras/sty3430.
- ^ López-Morales, Mercedes. On the Correlation between the Magnetic Activity Levels, Metallicities, and Radii of Low-Mass Stars. The Astrophysical Journal. May 2007, 660 (1): 732–739. Bibcode:2007ApJ...660..732L. S2CID 119530297. arXiv:astro-ph/0701702 . doi:10.1086/513142.
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- ^ ARICNS star page of Lacaille 9352. Astronomisches Rechen-Institut Heidelberg. [2010-04-16]. (原始内容存档于2012-09-16).
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