罗斯128
观测资料 历元 J2000 | |
---|---|
星座 | 室女座 |
星官 | |
赤经 | 11h 47m 44.3964s[1] |
赤纬 | +00° 48′ 16″[1] |
视星等(V) | 11.13[2] |
特性 | |
光谱分类 | M4 V[3] |
U−B 色指数 | 2.685[4] |
B−V 色指数 | 1.59[5] |
变星类型 | 闪焰星 |
天体测定 | |
径向速度 (Rv) | -13[6] km/s |
自行 (μ) | 赤经:605.66[1] mas/yr 赤纬:-1219.32[1] mas/yr |
视差 (π) | 299.59 ± 2.20[1] mas |
距离 | 10.89 ± 0.08 ly (3.34 ± 0.02 pc) |
绝对星等 (MV) | 13.51[2] |
详细资料 | |
质量 | 0.15[7] M☉ |
半径 | 0.21[8] R☉ |
表面重力 (log g) | 3.40[7] |
亮度 | 0.00029[来源请求] L☉ |
温度 | 3,180[3] K |
其他命名 | |
罗斯128是一颗红矮星,是恒星中第11靠近太阳系的恒星系,距离是10.89光年。它在1926年首度被法兰克·埃尔莫尔·罗斯记录在星表中[9]。
这是一颗老的银盘面星,这意味着它是低金属量星,并且轨道接近银河的平面[10]。由于它在数分钟内的周期内光度就会不可预知的显著增加,因此被分类为一颗活动中的闪焰星[11]。因为闪焰活动的频率不高,它被认为是一颗被磁化的恒星,也就是有一些证据显示恒星的星风有一些磁制动使闪焰的频率降低,但不能确认是否净效应[12]。
在研究这颗恒星的多个场合的案例中显示,这颗恒星有一颗伴星是低质量的棕矮星,在距离主星至少1天文单位的轨道上环绕者,但是迄今尚未发现任何伴星[13][14]。这颗恒星也缺乏额外的红外线辐射,而过量的红外线辐射通常是有尘埃环在轨道中环绕恒星的指标[15][16]。
罗斯128环绕银河的轨道与银河核心的距离从8.22至10.49千秒差距变化,轨道离心率是0.122[17]。这个轨道会使这颗恒星在未来会更接近太阳系,大约在71,000年之后,它与太阳系的距离大约是1.911 ± 0.026秒差距.[18]。
行星系统
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 | +0.56 −0.43 1.8M⊕ |
±0.0017 0.0493 | ±0.0056 9.8596 | ±0.092 0.036 | — | +1.1 −0.65 1.6R⊕ |
相关条目
参考资料
- ^ 1.0 1.1 1.2 1.3 1.4 1.5 Perryman, M. A. C.; et al. The HIPPARCOS Catalogue. Astronomy & Astrophysics. April 1997, 323: L49–L52. Bibcode:1997A&A...323L..49P.
- ^ 2.0 2.1 The One Hundred Nearest Star Systems. Research Consortium on Nearby Stars. 2009-01-01 [2009-09-03]. (原始内容存档于2012-05-14).
- ^ 3.0 3.1 Gautier, T. N.; et al. Far Infrared Properties of M Dwarfs. Bulletin of the American Astronomical Society: 1431. Bibcode:2004AAS...205.5503G.
- ^ Rufener, F. Second catalogue of stars measured in the Geneva Observatory photometric system. Astronomy & Astrophysics Supplement Series. October 1976, 26: 275–351. Bibcode:1976A&AS...26..275R.
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- ^ Wilson, Ralph Elmer, General catalogue of stellar radial velocities, Washington: Carnegie Institution of Washington, 1953, Bibcode:1953QB901.W495.....
- ^ 7.0 7.1 Rodonò, Marcello. The Atmospheres of M Dwarfs: Observations. Washington: NASA. : 409–453.
|booktitle=
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- ^ Jura, M.; et al. Mid-Infrared Spectra of Dust Debris around Main-Sequence Stars. The Astrophysical Journal Supplement Series. September 2004, 154 (1): 453–457. doi:10.1086/422975.
- ^ Gautier, Thomas N., III; et al. Far-Infrared Properties of M Dwarfs. The Astrophysical Journal. September 2007, 667 (1): 527–536. doi:10.1086/520667.
- ^ Allen, C.; Herrera, M. A. The galactic orbits of nearby UV Ceti stars. Revista Mexicana de Astronomia y Astrofisica. 1998, 34: 37–46 [2008-06-13]. (原始内容存档于2018-10-07).
- ^ García-Sánchez, J.; Weissman, P. R.; Preston, R. A.; Jones, D. L.; Lestrade, J.-F.; Latham, D. W.; Stefanik, R. P.; Paredes, J. M. Stellar encounters with the solar system. Astronomy and Astrophysics. 2001, 379: 634–659. doi:10.1051/0004-6361:20011330.
- ^ 引用错误:没有为名为
4-planet
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