Ross 128

罗斯128

Ross 128 is a dim, main-sequence red dwarf that is comparable to the brighter of the two stars, Gliese 623a, shown in the NASA HST image at left.

Ross 128 是一颗暗淡的主序星，其亮度与图中左侧 NASA HST 图像中所示的两颗星中较亮的一颗 Gliese 623a 相当。

"This dim star lies about 10.9 light-years (ly) away in the northeastern corner (11:47:44.40+00:48:16.43, ICRS 2000.0) of Constellation Virgo, the Maiden -- south of Zavijava (Beta Virginis). It is too faint to be seen with the naked eye. The star was discovered in 1925 by Frank Elmore Ross (1874-1960), who also took the first good infrared and ultraviolet photographs of Venus in 1923. Ross first reported on this star in his "Second List of New Proper-Motion Stars," Astronomical Journal (36:856)."(Solstation)

这颗暗星位于室女座（处女座）东北角（坐标11:47:44.40+00:48:16.43，ICRS 2000.0），距离约10.9光年，位于Zavijava（Beta Virginis）以南。由于太暗，无法用肉眼看到。这颗星于1925年由Frank Elmore Ross（1874-1960）发现，他同时也于1923年拍摄了金星的首次高质量红外线和紫外线照片。Ross首次报告这颗星是在他的《第二份新自行星列表》中，发表于《天文学期刊》（36:856）。

"This cool and dim, main sequence red dwarf (M4.1 Vn) has almost a third of Sol's mass, a tenth of its diameter, but only 33/100,000th of its luminosity. (Another reference suggests a tenth of Sol's mass, a fifth of its diameter, and 23/100,000 of its luminosity). Ross 128 would be only one of many unremarkable stars except that it appears to be a flare star as well as one of Sol's closest neighbors. In contrast to Proxima Centauri which is a "magnetically younger" flare star that is "activity saturated", however, Ross 128 is considered to be a more "evolved" flare star where its flare rate may have decreased somewhat with increased magnetic evolution (Andrew Skumanich, 1986)."(Solstation)

这颗凉爽暗淡的主序星红矮星（M4.1 Vn）的质量几乎只有太阳的三分之一，直径只有其十分之一，但其光度只有太阳的33/100000。（另一份资料指出其质量是太阳的十分之一，直径是其五分之一，光度是太阳的23/100000）。Ross 128只是众多不显眼的恒星之一，除非它同时被认定为一颗耀斑星，而且是太阳的近邻之一。与Proxima Centauri相比，后者是一颗“磁性更年轻”的耀斑星，且“活动已饱和”，然而Ross 128则被认为是一颗更“进化”的耀斑星，其耀斑频率可能随着磁活动的增强而有所降低（Andrew Skumanich, 1986）。

Sources:

http://www.solstation.com/stars/ross128.htm
Skumanich http://adsbit.harvard.edu/cgi-bin/nph-iarticle_query?1986ApJ...309..858S
Skumanich http://adsbit.harvard.edu/cgi-bin/nph-iarticle_query?1986ApJ...309..858S（专名或术语）

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Ross 154

罗斯154

Ross 154 is a dim, main-sequence red dwarf that is comparable to the two stars, Gliese 623a and the dimmer Gliese 623b, shown in the NASA HST image at left.

Ross 154 是一颗暗淡的主序星红矮星，其亮度与左图中所示的两颗恒星 Gliese 623a 和更暗的 Gliese 623b 相当。

"This dim star is the seventh closest to our Sun, lying at about 9.7 light-years (ly) away. It is located in the eastern part (18:49:49.36-23:50:10.44, ICRS 2000.0) of Constellation Sagittarius, the Archer -- northeast of Kaus Borealis (Lambda Sagittarii). However, Ross 154 is too faint to be seen by the naked eye. The star was discovered in 1925 by Frank Elmore Ross (1874-1960), who also took the first good infrared and ultraviolet photographs of Venus in 1923. Ross first reported on this star in his "Second List of New Proper-Motion Stars," Astronomical Journal (36:856)."(Solstation)

这颗暗淡的恒星是距离太阳第七近的恒星，位于约9.7光年（ly）之外。它位于天琴座（The Archer）的东部分区（坐标18:49:49.36-23:50:10.44，ICRS 2000.0），位于Kaus Borealis（Lambda Sagittarii）东北方向。然而，Ross 154太暗，无法用肉眼看到。这颗恒星于1925年由Frank Elmore Ross（1874-1960）发现，他同时在1923年拍摄了 Venus 的首次高质量红外线和紫外线照片。Ross 首次报告这颗恒星是在他的《第二份新自行星列表》中，发表于《天文学期刊》（36:856）。

"This cool and dim, main sequence red dwarf (M3.5 Ve) has around 17 percent of Sol's mass (RECONS estimate), 24 percent of its diameter (Johnson and Wright, 1983, page 693), and less than 5/10,000th of its luminosity. Ross 154 would be only one of many unremarkable stars except that it appears to be a flare star as well as one of Sol's closest neighbors. Its variable star designation is V1216 Sagittarii."(Solstation)

这颗凉爽而暗淡的主序星红矮星（M3.5 Ve）的质量约为太阳的17%（RECONS估计），直径约为太阳的24%（Johnson和Wright，1983，第693页），其光度则不到太阳的5/10,000。Ross 154只是众多不显眼的恒星之一，除非它同时是一颗耀斑星，而且还是太阳的近邻之一。它的变星编号是V1216 Sagittarii。

Sources:

http://www.solstation.com/stars/ross154.htm

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Ross 248

罗斯248

Ross 248 is a dim, main-sequence red dwarf that is comparable to the two stars, Gliese 623a and the dimmer Gliese 623b, shown in the NASA HST image at left.

Ross 248 是一颗暗淡的主序星红矮星，其亮度与左侧 NASA HST 图像中所示的两颗恒星 Gliese 623a 和更暗的 Gliese 623b 相当。

"Ross 248 lies about 10.3 light-years (ly) away in the northwestern part (23:41:54.0+44:09:32:C~, ICRS 2000.0) of Constellation Andromeda, the Chained Maiden -- south of Lambda Andromedae and near Kappa and Iota Andromedae. It is too faint to be seen by the naked eye. The star was discovered in 1925 by Frank Elmore Ross (1874-1960), who also took the first good infrared and ultraviolet photographs of Venus in 1923. Ross first reported on this star in his "Second List of New Proper-Motion Stars," Astronomical Journal (36:856)."(Solstation)

Ross 248 位于仙女座（Andromeda，The Chained Maiden）西北部（赤经23:41:54.0，赤纬+44:09:32，ICRS 2000.0），距离地球约10.3光年，位于Lambda Andromedae以南，接近Kappa和Iota Andromedae。由于太暗，无法用肉眼看到。这颗星于1925年由Frank Elmore Ross（1874-1960）发现，他还在1923年拍摄了Venus的首次高质量红外和紫外照片。Ross首次报告这颗星是在他的《第二份新自行星列表》中，发表于《天文学期刊》（36:856）。

"This cool and dim, main sequence red dwarf (M5.5 or 4.9 Ve) has almost a fourth of Sol's mass, seven percent of its diameter, but only 11/100,000th of its luminosity. (Another reference, however, suggests seven percent of Sol's mass, 17 percent of its diameter, but the same luminosity). Ross 248 would be only one of many unremarkable stars except that it is one of Sol's closest neighbors. Classified as a flare star, the star also has the variable designation HH Andromedae, and investigators have reported finding possible periods of variability at 4.2 years, 120 or 121 days, and five other periods between 60 and 291 days, which may be caused by an unresolved companion (Edward W. Weiss, 1993, page 1139)."(Solstation)

这颗凉爽而暗淡的主序红矮星（M5.5或4.9 Ve）的质量几乎只有太阳的四分之一，直径是太阳的7%，但其光度只有太阳的11/100,000。（然而，另一份资料却指出其质量是太阳的7%，直径是太阳的17%，但光度相同）。Ross 248只是众多不显眼的恒星之一，除非它是最接近太阳的邻居之一。该恒星被归类为耀星，也被称为HH Andromedae，研究者报告发现可能的变光周期为4.2年、120或121天，以及五个介于60至291天之间的其他周期，这可能由未分辨的伴星引起（Edward W. Weiss, 1993, 第1139页）。

Sources:

http://www.solstation.com/stars/ross248.htm

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