热海王星系统HD 106315的近$2:1$ 平运动共振捕获与轨道演化
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1.中国科学院紫金山天文台南京210023;2.中国科学院行星科学重点实验室南京210023;3.中国科学技术大学天文与空间科学学院合肥230026)

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P136;

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%\hangafter 1%\hangindent 2.5em国家自然科学基金项目(11773081、11873097、12033010), 中国科学院创新交叉团队项目和中国科学院紫金山天文台小行星基金会资助


Near $2:1$ Mean Motion Resonance Capture and Orbital Evolution of A Hot-Neptune System: HD 106315
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1. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023;2. Key Laboratory of Planetary Sciences, Chinese Academy of Sciences, Nanjing 210023;3. School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026;

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    摘要:

    通过结合理论分析和数值模拟方法, 可以对热海王星系统HD 106315轨道迁移中的近$2:1$平运动共振捕获机制以及潮汐作用下的演化过程进行研究. 在轨道迁移阶段, 初始轨道半长径、初始偏心率以及行星c的偏心率衰减系数K会对系统轨道构型产生影响. 数值模拟结果显示当初始轨道半长径分别为$a_b\sim 0.4$au、$a_c\sim 0.8$au, 偏心率$e_b$和$e_c$均小于0.03时, HD 106315b和HD 106315c在中央恒星的引力作用以及原行星盘粘滞作用下向内迁移, 65000 yr左右两颗行星均可迁移至当前观测位置附近并形成近$2:1$平运动共振捕获. 此外, 中央恒星的潮汐效应也可能会对行星系统共振构型产生影响, 理论分析表明当行星潮汐耗散系数$Q=100$时, 潮汐效应造成的轨道半长径衰减使系统轨道周期比发生的变化可能是系统脱离共振构型的原因. 数值模拟结果显示, HD 106315系统内两颗行星 $Q\geqslant 10^3$时, 来自中央恒星的潮汐效应并不会使行星系统产生明显的偏心率和轨道半长径衰减, 不足以使HD 106315行星系统在剩余寿命内脱离$2:1$平运动共振轨道构型.

    Abstract:

    In this work, we investigate the near $2:1$ mean motion resonance capture scenario and tidal evolution for the hot-Neptune system HD 106315 by numerical simulations. To make a deeper understanding of migration for this system, we extensively explore the initial semi-major axis, eccentricity, as well as the attenuation coefficient of the eccentricity of HD 106315c affecting the orbital configuration of the system. The numerical simulations show that when the initial orbital elements of two planets are $a_b\sim0.4$au, $a_c\sim0.8$au, $e_b$ and $e_c$ lower than 0.03, HD 106315b and HD 106315c can migrate to currently observed location, and form near $2:1$ mean motion resonance. This scenario takes into account the effect of the central star and the viscosity of disk.\qquad In addition, tidal dissipation that originates from the host star, can influence the mean motion resonant configuration for planets. From a viewpoint of theoretical analysis and simulations, the results show that for tidal dissipation factor $Q = 100 $, the ratio of orbital period of two planets will change over the evolution. This may be indicative of the resonant departure for two planets in the system. However, tidal dissipation factor Q may be larger than $10^3$ for the planets, therefore we may safely conclude that tidal effect does not play a major role in driving two Neptunian planets of the HD 106315 system move out of $2:1$ mean motion resonance within the residual lifetime of the star.

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黄秀敏,季江徽,董瑶.热海王星系统HD 106315的近$2:1$ 平运动共振捕获与轨道演化[J].天文学报,2020,(5):75-89.

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  • 收稿日期:2020-01-18
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  • 在线发布日期: 2020-09-29
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