The influence of binary interactions on infrared passbands of populations
The influence of binary interactions on infrared passbands of populations
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DOI：
10.1111/j.1365-2966.2008.14280.x
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发表时间：
2009-06
影响因子：
4.8
通讯作者：
Fenghui Zhang;Lifang Li;Zhanwen Han
中科院分区：
文献类型：
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作者：
Fenghui Zhang;Lifang Li;Zhanwen Han
在我们的进化星群合成模型中，双星的样本通过“修补”蒙特卡罗模拟再现，恒星质量、J、H、K、L、L2和M等的综合星等、质量光比和涉及红外波段的宽颜色被呈现在一组广泛的瞬时爆发双星星群中。此外，还减少了Zhang等人给出的集成颜色的波动。通过比较有（模型A）和没有（模型B）相互作用的双星群的结果，我们表明，包括双星相互作用使双星群的恒星质量更小（类似于过去15 Gyr期间的3.6% - 4.5%），星等更大（除了U，最多类似于0.18等），除了金属丰度较高的U和B波段外，颜色更蓝（类似于V - K波段的最高0.15等），质量光比更大（类似于K波段的0.06等）。二元相互作用使V等对年龄不太敏感，而R和I等对金属丰度更敏感。给定年龄，模型A和B之间的恒星质量、星等和质量光比（U和B波段除外）差异的绝对值在Z = 0.0001处达到最大值，即双星相互作用对这些参数的影响达到最大值，而某些颜色的差异在Z处达到最大值，类似于0.01-0.0004。相比之下，恒星质量差的绝对值在Z = 0.03时最小；U、B、V等的质光比在Z处达到最小值，约为0.01 ~ 0.004。
In our evolutionary population synthesis models, samples of binaries are reproduced by a 'patched' Monte Carlo simulation and the stellar masses, integrated J, H, K, L, L2 and M magnitudes, mass-to-light ratios and broad colours involving infrared bands are presented for an extensive set of instantaneous-burst binary stellar populations. In addition, the fluctuations in the integrated colours, which have been given by Zhang et al., are reduced. By comparing the results for binary stellar populations with (Model A) and without (Model B) binary interactions, we show that the inclusion of binary interactions makes the stellar mass of a binary stellar population smaller (similar to 3.6-4.5 per cent during the past 15 Gyr), magnitudes greater (except U, similar to 0.18 mag at the most), colours bluer (similar to 0.15 mag for V - K at the most) and mass-to-light ratios greater (similar to 0.06 for K band) except those in the U and B passbands at higher metallicities. Binary interactions make the V magnitude less sensitive to age, and R and I magnitudes more sensitive to metallicity. Given an age, the absolute values of the differences in the stellar mass, magnitudes and mass-to-light ratios (except those in the U and B bands) between Models A and B reach a maximum at Z = 0.0001, i. e. the effects of binary interactions on these parameters reach a maximum, while the differences in some colours reach a maximum at Z similar to 0.01-0.0004. In contrast, the absolute value of the difference in the stellar mass is minimal at Z = 0.03; those in the U, B, V magnitudes and the mass-to-light ratios in the U and B bands reach a minimum at Z similar to 0.01-0.004.