论文标题
Lamost-MRS调查中二进制的质量比分布
Mass-Ratio Distribution of Binaries From the LAMOST-MRS Survey
论文作者
论文摘要
二元进化导致形成对天体物理学发展至关重要的重要物体的形成，但是二元种群的统计特性仍然很少了解。 Lamost-MRS提供了大量恒星样本来研究二元种群的性质，尤其是对于质量比分布和二元分数。我们已经设计了一种峰值振幅比（PAR）方法，以根据从其光谱获得的结果来得出二进制系统的质量比。通过计算互相关函数（CCF），我们建立了派生的质量比与二进制系统的PAR之间的关系。通过利用从Lamsot DR6和DR7获得的光谱观测值，我们应用了PAR方法来形成二元系统与光谱类型的派生质量比的分布。我们选择了质量比0.6-1.0 $ $ $的质量比率来研究质量比率分布。通过幂律拟合，我们分别在样品中确定的A-，F-，F-和G-Type明星分别获得了$ -0.42 \ pm0.27 $，$ 0.03 \ pm0.12 $的功率指数$γ$值。派生的$γ$价值表现出越来越多的趋势趋于较低的一级恒星质量，而G-Type二进制型在双胞胎中的趋势往往更多。近距离二进制分数（对于$ p \ lyssim 150 \，{\ rm d} $和$ q \ gtrsim 0.6 $在我们的样品中，对于A，F和G二元组为$ 7.6 \ pm 0.5 \％$，$ 4.9 \ $ 4.9 \ pm 0.2 \ pm 0.2 \％$ $ 3.7 \ $ 3.7 \ $ 3.7 \ $ 0.1 \ pm 0.1 \％\％\％\％\％\％\％\％\％\％相应。请注意，可以将PAR方法应用于恒星的大型光谱调查。
Binary evolution leads to the formation of important objects crucial to the development of astrophysics, but the statistical properties of binary populations are still poorly understood. The LAMOST-MRS has provided a large sample of stars to study the properties of binary populations, especially for the mass ratio distributions and the binary fractions. We have devised a Peak Amplitude Ratio (PAR) approach to derive the mass ratio of a binary system based on results obtained from its spectrum. By computing a cross-correlation function (CCF), we established a relationship between the derived mass ratio and the PARs of the binary systems. By utilizing spectral observations obtained from LAMSOT DR6 & DR7, we applied the PAR approach to form distributions of the derived mass ratio of the binary systems to the spectral types. We selected the mass ratio within the range of $0.6-1.0$ for investigating the mass-ratio distribution. Through a power-law fitting, we obtained the power index $γ$ values of $-0.42\pm0.27$, $0.03\pm0.12$, and $2.12\pm0.19$ for A-, F-, and G-type stars identified in the sample, respectively. The derived $γ$-values display an increasing trend toward lower primary star masses, and G-type binaries tend to be more in twins. The close binary fractions (for $P\lesssim 150\,{\rm d}$ and $q\gtrsim 0.6$) in our sample for A, F and G binaries are $7.6\pm 0.5 \%$, $4.9\pm 0.2 \%$ and $3.7 \pm 0.1 \%$, respectively. Note that the PAR approach can be applied to large spectroscopic surveys of stars.
