Wide binaries in the Orion nebula cluster
Wide binaries in the Orion nebula cluster
复制标题
猎户座星云团中的宽双星
DOI：
10.1046/j.1365-8711.1999.02513.x
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发表时间：
1999
影响因子：
4.8
通讯作者：
H Germany
中科院分区：
文献类型：
--
作者：
A. Scally;C. Clarke;M. T. I. F. Astronomy;Cambridge;UK.;A. Potsdam;H Germany
利用Jones & Walker在1988年编制的猎户座星云星团（ONC）中894颗恒星的适当运动数据，我们搜索了距离在1000-5000天文单位范围内的双星，并找到了3颗的上限。使用蒙特卡罗方法，我们用两个假设来检验这个结果的一致性：i)星团包含一个与太阳附近发现的相同的双星群，ii)在这个分离范围内星团根本不包含双星群。我们得到的结果强烈支持后一种假设。
Using proper motion data for 894 stars in the Orion Nebula Cluster (ONC) compiled by Jones & Walker in 1988, we search for binaries with apparent separations in the range 1000-5000 AU, and find an upper limit of three. Using a Monte Carlo method, we test the consistency of this result with two hypotheses: i) that the cluster contains a binary population identical to that found in the solar neighbourhood, and ii) that the cluster contains no binaries at all in this separation range. We obtain results strongly favouring the latter hypothesis.
Star formation in the Galaxy is seen to occur in a variety of different environments, but it has been proposed that most stars may be formed in dense regions similar to the ONC, rather than in less dense groupings like that found in Taurus-Auriga. Since roughly 15 per cent of galactic field stars are known to be in binaries with separations greater than 1000 AU, the apparent absence of such binaries in the ONC places an upper limit on the contribution that dense clusters can make to galactic star formation.