行星半径对类金星行星氧离子逃逸比例长期演化的影响
doi: 10.11728/cjss2026.03.2025-0090 cstr: 32142.14.cjss.2025-0090
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王鑫珂 男, 2000年1月出生于河南省许昌市, 毕业于中国科学院国家空间科学中心, 主要研究方向为空间等离子体模拟. E-mail: 1210763881@qq.com -
李海涛 男, 1982年9月出生于山东省济宁市, 现为中国科学院国家空间科学中心副研究员, 英国埃克塞特大学访问学者, 主要研究方向为系外行星探测与物理. E-mail: lihaitao@nssc.ac.cn
作者简介:
通讯作者:
Effects of Planet Radius on Long-term Evolution of Oxygen Ion Escape Proportion in Venus-like Planets
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摘要: 近年来已发现数千颗系外行星, 并对这些行星的大气成分、轨道特性、宜居性等特性展开了深入研究. 恒星与行星大气的相互作用被认为是影响行星大气演化及其宜居性的核心机制之一. 本研究旨在揭示行星半径在其大气逃逸长期演化中的作用, 通过建立三维磁流体动力学模型, 结合恒星系统演化特征, 并基于类金星大气逃逸模型, 以Kepler-1649 c及其宿主恒星的参数作为样本, 假设一颗具有类金星大气的行星作为研究对象, 构建了涵盖不同行星半径和恒星年龄的数值模拟体系. 研究发现行星半径会显著改变各离子的逃逸比例, O+的逃逸率占总逃逸率的比例随行星半径的增大而减小. 本研究揭示了行星半径对离子逃逸行为的差异性影响, 为理解系外行星大气演化提供了新视角.Abstract: In recent years, the study of exoplanets has become a hot topic in astronomy and planetary science. With the rapid development of detection technology, mankind has discovered and confirmed thousands of exoplanets, and has carried out in-depth studies on the atmospheric composition, orbital properties, habitability and other key characteristics of these exoplanets. In this context, star-planet atmosphere interactions have been recognized as one of the central mechanisms affecting the evolution of planetary atmospheres and their habitability. In this study, we aim to reveal the role of planetary radii in the long-term evolution of their atmospheric escape. By building a three-dimensional Magnetohydrodynamic (MHD) model and combining it with the evolutionary characteristics of the stellar system, we reveal the role of planetary radii in the long-term evolution, and construct a numerical simulation system based on the Venus-like atmospheric escape model, taking the characteristic parameters of Kepler-1649 c and its host star as a sample, it is assumed that a planet with Venus-like atmosphere is used as the research object, which covers different planetary radii and stellar ages. It is found that the planetary radius significantly changes the escape contribution ratio of each ion. Among them, the escape rate of O+ as a proportion of the total escape rate decreases with increasing planetary radius, from 99.3% to 17.1% at 4.8 Ga. Meanwhile, the variability between the O+ ion distribution and the total ion distribution in interplanetary space increases with radius. This study provides a new perspective for understanding the mechanism of exoplanet atmospheric evolution by discovering the differential effect of planetary radius on the escape behavior of different ions.
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Key words:
- MHD simulation /
- Space plasma /
- Exoplanets /
- Ion escape
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图 2 不同条件下氧离子逃逸率比例随年龄的变化
Figure 2. Proportion of the oxygen ion escape rate as a function of age under different conditions
图 3 0.7 Ga时不同行星半径下氧离子和总离子在行星际空间中的分布
Figure 3. Distribution of oxygen ions and total ions in the interplanetary space at 0.7 Ga with different planetary radii
图 4 4.8 Ga时不同行星半径下氧离子和总离子在行星际空间中的分布
Figure 4. Distribution of oxygen ions and total ions in the interplanetary space at 4.8 Ga with different planetary radii
表 1 金星离子逃逸化学反应网络[23]
Table 1. Chemical reactions network for ion escape from Venus
化学反应 反应速率 $ {\text{CO}}_{2}\text{+h}\nu \to \text{CO}_{2}^{+}\text{+e} $ 见表2 $ \text{O+h}\nu \to {\text{O}}^{+}\text{+e} $ 见表2 $ \text{CO}_{2}^{+}+\mathrm{O}\rightarrow \mathrm{O}_{2}^{+}+\text{CO} $ $ 1.64 \times 10^{-10} \mathrm{cm}^{-3} \cdot \mathrm{s}^{-1} $ $ \text{CO}_{2}^{+}+\mathrm{O}\rightarrow {\mathrm{O}}^{+}+{\text{CO}}_{2} $ $ 9.60 \times 10^{-11} \mathrm{cm}^{-3} \cdot \mathrm{s}^{-1} $ $ {\mathrm{O}}^{+}+\mathrm{CO}\rightarrow \mathrm{O}_{2}^{+}+\text{CO} $ $ 1.1 \times 10^{-9}\left(800 / T_{{\mathrm{e}}}\right)^{0.39} \mathrm{cm}^{-3} \cdot \mathrm{s}^{-1} $ $ {\mathrm{H}}^{+}+\mathrm{O}\rightarrow {\mathrm{O}}^{+}+\mathrm{H} $ $ 3.75 \times 10^{-10} \mathrm{cm}^{-3} \cdot \mathrm{s}^{-1} $ $ \mathrm{O}_{2}^{+}+\mathrm{e}\rightarrow \mathrm{O}+\mathrm{O} $ $ 7.38 \times 10^{-8}\left(1200 / T_{{\mathrm{e}}}\right)^{0.56} \mathrm{cm}^{-3} \cdot \mathrm{s}^{-1} $ $ \text{CO}_{2}^{+}+\mathrm{e}\rightarrow \mathrm{CO}+\mathrm{O} $ $ 3.50 \times 10^{-7}\left(300 / T_{{\mathrm{e}}}\right)^{0.5} \mathrm{cm}^{-3} \cdot \mathrm{s}^{-1} $ 
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表 2 恒星风参数、行星际磁场和光电离率
Table 2. Stellar wind parameters, the interplanetary magnetic field and the photoionization rate
年龄/Ga 太阳风密度/
cm–3太阳风温度
(×106) / K太阳风速度/
(km·s–1)行星际磁场/nT 二氧化碳光电离率
(×10–5) / s–1氧原子光电离率
(×10–5) / s–10.7 964 2.01 (–684, 0, 0) (–144.732, –0.230,0) 3.75 1.41 1.0 583 1.59 (–580, 0, 0) (–123.843, –0.169,0) 3.75 1.41 1.5 328 1.22 (–484, 0, 0) (–104.446, –0.118,0) 3.75 1.41 2.0 218 1.01 (–425, 0, 0) (–92.509, –0.091,0) 2.78 1.04 2.5 159 0.869 (–384, 0, 0) (–83.557, –0.074,0) 1.99 0.747 3.0 123 0.771 (–353, 0, 0) (–77.588, –0.063,0) 1.51 0.5.68 3.5 99 0.697 (–328, 0, 0) (–74.604, –0.056,0) 1.20 0.451 4.0 82 0.639 (–308, 0, 0) (–70.128, –0.049,0) 0.982 0.369 4.5 69 0.591 (–292, 0, 0) (–67.144, –0.044,0) 0.8.23 0.309 4.8 63 0.567 (–283, 0, 0) (–64.160, –0.041,0) 0.7.47 0.281
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表 3 行星半径以及相应的质量
Table 3. Radii of planets and their corresponding masses
半径/$ {R}_{\text{p}} $ 半径值/km 质量 (×1024)/kg 0.50 3392 0.564 0.75 5088 2.528 1.00 6784 7.330 1.25 8480 16.74 1.50 10176 32.86 1.75 11972 58.12 2.00 13568 95.26
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