| 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]。
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. 1997-04, 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].
- ↑ 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. 1976-10, 26: 275–351. Bibcode:1976A&AS...26..275R.
- ↑ Warren, W. H., Jr. Photoelectric Photometric Catalogue of Homogeneous Means in the UBV System. Observatory (Geneva). 1978.
- ↑ 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=被忽略 (帮助) - ↑ White, Stephen M.; Jackson, Peter D.; Kundu, Mukul R. A VLA survey of nearby flare stars. Astrophysical Journal Supplement Series. 1989-12, 71: 895–904. doi:10.1086/191401.
- ↑ Ross, Frank E. New proper-motion stars, (second list). Astronomical Journal: 124–128. doi:10.1086/104699.
- ↑ Sánchez, F. Vazquez, M. , 编. New windows to the universe 2. Cambridge University Press. 1990: 313. ISBN 052138429X.
- ↑ Kunkel, W. E. Solar neighborhood flare stars - A review. Variable stars and stellar evolution; Proceedings of the Symposium. Moscow, USSR: D. Reidel Publishing Co: 15–46. July 29-August 4, 1974. Bibcode:1975IAUS...67...15K.
- ↑ Skumanich, Andrew. Some evidence on the evolution of the flare mechanism in dwarf stars. Astrophysical Journal, Part 1. 1986-10-15, 309: 858–863. doi:10.1086/164654.
- ↑ Hinz, Joannah L.; McCarthy, Donald W., Jr.; Simons, Doug A.; Henry, Todd J.; Kirkpatrick, J. Davy; McGuire, Patrick C. A Near-Infrared, Wide-Field, Proper-Motion Search for Brown Dwarfs. The Astronomical Journal. 2002-04, 123 (4): 2027–2032. doi:10.1086/339555.
- ↑ Schroeder, Daniel J. A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2. The Astronomical Journal. 2000, 119: 906–922. doi:10.1086/301227.
- ↑ Jura, M.; et al. Mid-Infrared Spectra of Dust Debris around Main-Sequence Stars. The Astrophysical Journal Supplement Series. 2004-09, 154 (1): 453–457. doi:10.1086/422975.
- ↑ Gautier, Thomas N., III; et al. Far-Infrared Properties of M Dwarfs. The Astrophysical Journal. 2007-09, 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].
- ↑ 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.
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