Initial conditions for the article "Survival of satellites during the migration of a Hot Jupiter"
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This repository contains the initial conditions to reproduce the results of the article: "Survival of satellites during the migration of a Hot Jupiter". These simulations were done with Posidonius (https://github.com/marblestation/posidonius/), version commit b3c5c71 (20/02/2022). To reproduce the results corresponding to the Equilibrium tide section (4.1), the two lines 20 & 21 in src/effects/tides/constant_time_lag.rs have to be commented and the code should be re-compiled before execution. By default, the dynamical tide is considered in both star and planet. The data file for the planet (evolution of the structure, following Leconte & Chabrier, 2013 [1]), including the dynamical tide dissipation as described in Section 2.3.3 is called Jupiter.dat. The initial conditions cover the following cases: a disk density of $\Sigma_0 = $1000 g/cm$^2$ disk lifetimes of 5'000, 7'000, 10'000, 12'500, 20'000, 35'000, 50'000 yr initial semi-major axis of the satellite of 0.3, 0.4, 0.6, 0.8, 1.0 $a_\mathrm{Io}$ (where $a_\mathrm{Io}$ is the distance between Jupiter and Io) masses of the satellite of 1 $M_\mathrm{Io}$ and 10 $M_\mathrm{Io}$ (where $M_\mathrm{Io}$ is the mass of Io) dissipations in the satellite of: $0$, $10^{-4}$, $10^{-2}$, $10^{-1}$, $1.0\times \Delta t_{\oplus}$ (where $\Delta t_\oplus$ is the time lag of the Earth) initial stellar rotation periods of 1~day, 3~days and 8~days The names of the initial conditions files contained in the Initial_conditions folder are as such: diskd_1000.0_gcm2_t50000_10.0_mIO_0.8_aIO_dissipFactor_1.0_rots_3.0.json For that specific example: the disk density $\Sigma_0$ is 1000 g/cm$^2$ the disk lifetime is 50'000 yr the mass of the satellite is 10 $M_\mathrm{Io}$ the initial satellite distance is 0.8 $a_\mathrm{Io}$ the dissipation factor (time lag) $\Delta t = 1.0 \Delta t_\oplus$ the initial rotation of the star is 3 days References: [1] Leconte, J. and Chabrier, G.~2013, Layered convection as the origin of Saturn's luminosity anomaly, Nature Geoscience, 6, 347, doi: 10.1038/ngeo1791 (https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L)
本仓库包含复现论文《热木星迁移过程中卫星的存续》（Survival of satellites during the migration of a Hot Jupiter）研究结果所需的初始条件。 本系列模拟基于Posidonius（https://github.com/marblestation/posidonius/）的b3c5c71版本提交（2022年2月20日）完成。若需复现平衡潮汐（Equilibrium tide）章节（4.1）的结果，需先注释src/effects/tides/constant_time_lag.rs文件中的第20、21行代码，重新编译后再运行模拟。默认配置下，恒星与行星均采用动力学潮汐（dynamical tide）模型。 用于存储行星结构演化（遵循Leconte与Chabrier 2013年的研究[1]）、并包含2.3.3节所述动力学潮汐耗散过程的数据集文件名为Jupiter.dat。 本次初始条件涵盖以下参数组合： 1. 盘面密度$Sigma_0=1000$ g/cm² 2. 盘面寿命分别为5000、7000、10000、12500、20000、35000、50000年 3. 卫星初始半长轴为0.3、0.4、0.6、0.8、1.0倍木卫一轨道半长轴$a_mathrm{Io}$（其中$a_mathrm{Io}$指木星与木卫一之间的轨道距离） 4. 卫星质量分别为1倍木卫一质量$M_mathrm{Io}$与10倍$M_mathrm{Io}$（其中$M_mathrm{Io}$为木卫一的质量） 5. 卫星的耗散参数取值为：0、$10^{-4}$、$10^{-2}$、$10^{-1}$、$1.0 imesDelta t_oplus$（其中$Delta t_oplus$为地球的时间延迟参数） 6. 恒星初始自转周期分别为1天、3天与8天 Initial_conditions文件夹内的初始条件文件命名规则如下：以diskd_1000.0_gcm2_t50000_10.0_mIO_0.8_aIO_dissipFactor_1.0_rots_3.0.json为例，该文件名对应的参数为： - 盘面密度$Sigma_0$为1000 g/cm² - 盘面寿命为50000年 - 卫星质量为10倍$M_mathrm{Io}$ - 卫星初始轨道距离为0.8倍$a_mathrm{Io}$ - 耗散因子（时间延迟）$Delta t=1.0Delta t_oplus$ - 恒星初始自转周期为3天 参考文献：[1] Leconte, J. 与 Chabrier, G. 2013, 《分层对流作为土星光度异常的成因》（Layered convection as the origin of Saturn's luminosity anomaly），《自然·地球科学》，第6卷，第347页，DOI: 10.1038/ngeo1791（链接：https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L）
