We present a comprehensive investigation of main-sequence binaries in the DRAGON simulations, which are the first one-million-particle direct N-body simulations of globular clusters. We analyze the orbital parameters of the binary samples in two of the DRAGON simulations, D1-R7-IMF93 and D2-R7-IMF01, focusing on their secular evolution and correlations up to 12 Gyr. These two models have different initial stellar mass functions: Kroupa 1993 (D1-R7-IMF93) and Kroupa 2001 (D2-R7-IMF01); and different initial mass-ratio distributions: random paring (D1-R7-IMF93) and a power law (D1-R7-IMF93). In general, the mass ratio of a population of binaries increases over time due to stellar evolution, which is less significant in D2-R7-IMF01. In D1-R7-IMF93, primordial binaries with a mass ratio q≈0.2 are most common, and the frequency linearly declines with increasing q at all times. Dynamical binaries of both models have higher eccentricities and larger semimajor axes than primordial binaries. They are preferentially located in the inner part of the star cluster. Secular evolution of binary orbital parameters does not depend on the initial mass-ratio distribution, but is sensitive to the initial binary distribution of the system. At t=12 Gyr, the binary fraction decreases radially outwards, and mass segregation is present. A color difference of 0.1 mag in F330W − F814W and 0.2 mag in NUV − y between the core and the outskirts of both clusters is seen, which is a reflection of the binary radial distribution and the mass segregation in the cluster. The complete set of data for primordial and dynamical binary systems at all snapshot intervals is made publicly available.

我们对DRAGON模拟中的主序列二元进行了全面的研究，这是第一个球状星团的一百万个粒子直接N体模拟。我们在两个DRAGON模拟中（D1-R7-IMF93和D2-R7-IMF01）分析了二元样品的轨道参数，重点是它们的长期演化和高达12 Gyr的相关性。这两个模型具有不同的初始恒星质量函数：Kroupa 1993（D1-R7-IMF93）和Kroupa 2001（D2-R7-IMF01）；以及不同的初始质量比分布：随机配对（D1-R7-IMF93）和幂律（D1-R7-IMF93）。通常，由于恒星的演化，二进制二进制数的质量比随时间增加，这在D2-R7-IMF01中不那么重要。在D1-R7-IMF93中，质量比为q的原始二进制≈0.2是最常见的，并且频率始终随q的增加线性下降。两种模型的动态二进制文件都比原始二进制文件具有更高的偏心率和更大的半长轴。它们优先位于星团的内部。二进制轨道参数的长期演化不取决于初始质量比分布，但对系统的初始二进制分布很敏感。在t = 12 Gyr时，二元分数沿径向向外减小，并且存在质量偏析。F330W-F814W中的色差为0.1 mag，而NUV - y中的色差为0.2 mag可以看到两个星团的核心和郊区之间的距离，这反映了星团中的二元径向分布和质量偏析。公开提供了所有快照间隔的原始和动态二进制系统的完整数据集。