二元相互作用对粒子群红外通带的影响
The Influence of Binary Interactions in Infrared passbands of populations
摘要：
在我们的演化星族合成模型中，双星的样本由"补丁"蒙特卡罗模拟再现，并给出了一组广泛的瞬时爆发双星恒星星族的恒星质量、J、H、K、L、L2和M等综合星等、质光比和包括红外波段在内的宽颜色。此外，Zhang等人（2005）给出的积分颜色的波动也减少了。通过比较有（模型A）和无（模型B）双星相互作用的双星恒星星族的结果，我们发现双星相互作用的加入使双星恒星星族的恒星质量变小（过去15 Gyr期间约为3.6 - 4.5%）;震级更大（U除外，最多~0.18mag）;颜色较小（V-K最多~0.15mag）;质光比较大（K波段~0.06），除了在高金属丰度的U和B通带。而且，二元相互作用使V星等对年龄不太敏感，R和I星等对金属丰度更敏感。给定一个年龄，模型A和B之间恒星质量、星等、质光比（U和B波段除外）之差的绝对值在Z = 0.0001处达到最大值，即，在Z~0.01 - 0.0004范围内，二元相互作用对这些参数的影响达到最大值，而某些颜色的差异达到最大值。相反，恒星质量差的绝对值在Z = 0.03时最小，U、B、V星等差和U、B波段的质光比在Z = 0.01~0.004时最小。
英文摘要：
In our evolutionary population synthesis models, the samples of binaries are reproduced by the '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. (2005), 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 (~3.6-4.5% during the past 15Gyr); magnitudes greater (except U, ~0.18mag at the most); colours smaller (~0.15mag for V-K at the most); the mass-to-light ratios greater (~0.06 for K-band) except those in the U and B passbands at higher metallicities. And, Binary interactions make the V magnitude less sensitive to age, R and I magnitudes more sensitive to metallicity. Given an age, the absolute values of the differences in the stellar mass, magnitudes, mass-to-light ratios (except those in the U and B bands) between Models A and B reach the maximum at Z=0.0001, i.e., the effects of binary interactions on these parameters reach the maximum, while the differences in some colours reach the maximum at Z ~0.01-0.0004. On the contrary, 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 the minimum at Z ~0.01-0.004.
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