The widest two components of the sy

The widest two components of the system are easily separated when viewed through binoculars, or even with the naked eye under excellent conditions.[1] The northern component is called ε1 and the southern one is called ε2; they both lie around 162 light years from Earth and orbit each other. When viewed at higher magnifications, both stars of the binary can be further split into binaries; that is, the system contains two sets of binary stars orbiting each other. Being able to view the components of each is a common benchmark for the resolving power of telescopes, since the individual doubles are so close together: the stars of ε1 were 2.35 arc-seconds apart in 2006, those of ε2 were separated by about the same amount in that year. Since the first high-precision measurements of their orbit in the 1980s, both binaries have moved only a few degrees in position angle.

The component stars of ε1 have magnitudes of 4.7 and 6.2 separated by 2.6" and have an orbital period that can only be crudely estimated at 1200 years, which places them at roughly 140 AU apart. The component stars of ε2 have magnitudes 5.1 and 5.5 separated by 2.3", and orbit in perhaps half that period. ε1 and ε2 themselves are not closer than 0.16 light years apart, and would take hundreds of thousands of years to complete an orbit. An observer at one pair would see the other pair shining with the light of a quarter Moon (which is about mv = −5.0), less than a degree away from each other.[2][3]

A fifth component of this system, orbiting one of the ε2 pair, was detected by speckle interferometry in 1985 and confirmed in two subsequent observations. No orbit can be prepared from such limited data, but its rapid motion suggests a period of a few tens of years. Its maximum observed separation of 0.2 arc-seconds precludes direct visual observation.

A number of other nearby stars may also be part of the system, bringing the system to a total of ten stars. The arrangement of the system is summarised in the tables below.

結果 (中文) 3:

最宽的两部件系统的易分离，通过望远镜观察时，甚至在良好的条件下肉眼。[ 1 ]北部的部分叫做ε1和南部的一个叫ε2；他们都躺在162光年来自地球和轨道彼此。当在高倍镜的二元恒星可以进一步分为二进制文件；即系统包含两套双星相互绕转。能够查看每个组件是望远镜的分辨力的共同基准，由于个人的双打是如此接近：1的ε星星2.35弧秒，除了在2006，2的ε相隔大约相同数量的那一年。自20世纪80年代以来的第一个高精度测量轨道，这两个二进制文件已经移动了只有几度的位置角。1部分对ε星星有4.7和6.2的幅度由2.6分离”并且有轨道周期，只能粗略地估计在1200年，这使他们分开约140金。2的ε组成恒星有5.1级和5.5隔2.3”，和轨道也许一半的时间。1、2εε本身不超过0.16光年的距离，并将成百上千年才能完成一个轨道。在一对一的观察者将看到另一对闪亮的月亮的光（这是−MV = 5），低于一定程度相互远离。[ 2 ] [ 3 ]该系统的五分之一个组成部分，轨道的一个ε2对，由1985散斑干涉检测，在随后的两个观测证实。没有轨道可以从这样有限的数据准备，但它的快速运动表明了几十年的一个时期。最大观察0.2弧秒的分离无法直接观察。许多其他附近的恒星也可能是系统的一部分，使系统，共十颗星。这种制度安排在下表概述。