A thermophysical analysis of the (1862) Apollo Yarkovsky and YORP effects
A thermophysical analysis of the (1862) Apollo Yarkovsky and YORP effects
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(1862) Apollo Yarkovsky 和 YORP 效应的热物理分析
DOI：
10.1051/0004-6361/201321659
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发表时间：
2013
影响因子：
6.5
通讯作者：
Rozitis B
中科院分区：
文献类型：
--
作者：
Rozitis B
引起轨道漂移的雅可夫斯基效应和引起自转速率和极方向变化的YORP效应在小行星的动力学和物理演化中发挥着重要作用。近地小行星（1862）阿波罗对轨道半长轴漂移和旋转加速度都有很强的探测能力。目标我们产生一个统一的模型，可以使用一组来自地面观测的热物理特性精确匹配这两种观测到的效应，并确定阿波罗的长期演化。方法我们使用光曲线形状反演技术和先进的热物理模型 （ATPM）根据已发布的光曲线、热红外和雷达观测结果来限制阿波罗的热物理特性。导出的属性用于对阿波罗的雅可夫斯基效应和 YORP 效应进行详细预测，然后与已发布的轨道漂移和旋转加速度测量结果进行比较。 ATPM 在模型预测中明确纳入了一维热传导、阴影、太阳光多重散射、全局自加热和粗糙表面热红外光束。结果我们发现 ATPM 可以准确地再现阿波罗的光曲线、热红外和雷达观测结果，并同时匹配观测到的轨道漂移和旋转加速度，使用：轴比为 的形状模型 1.94:1.65:1.00，有效直径1.55±0.07 km，几何反照率0.20±0.02，热惯性140-100+140J m-2K-1s−1/2，表面高度粗糙，堆积密度2850-680+480kg m-3。利用这些特性，我们预测阿波罗的倾角正以每 105 年 1.5-0.5+0.3 度的速率向 180° YORP 渐近状态增加。结论推导出的热惯性表明阿波罗的表面有松散的风化层材料，这与阿波罗最近根据其观测到的 Q 型光谱经历的表面重整事件一致。推断的体积密度与其他 S 型小行星确定的体积密度一致，表明阿波罗的内部有裂缝。 YORP 效应的作用时间比雅可夫斯基效应快得多，并将主导阿波罗的长期演化。 ATPM 可以很容易地应用于具有类似观测数据集的其他小行星。
ContextThe Yarkovsky effect, which causes orbital drift, and the YORP effect, which causes changes in rotation rate and pole orientation, play important roles in the dynamical and physical evolution of asteroids. Near-Earth asteroid (1862) Apollo has strong detections of both orbital semimajor axis drift and rotational acceleration.AimsWe produce a unified model that can accurately match both observed effects using a single set of thermophysical properties derived from ground-based observations, and we determine Apollo’s long term evolution.MethodsWe use light-curve shape inversion techniques and the advanced thermophysical model (ATPM) on published light-curve, thermal-infrared, and radar observations to constrain Apollo’s thermophysical properties. The derived properties are used to make detailed predictions of Apollo’s Yarkovsky and YORP effects, which are then compared with published measurements of orbital drift and rotational acceleration. The ATPM explicitly incorporates 1D heat conduction, shadowing, multiple scattering of sunlight, global self-heating, and rough surface thermal-infrared beaming in the model predictions.ResultsWe find that ATPM can accurately reproduce the light-curve, thermal-infrared, and radar observations of Apollo, and simultaneously match the observed orbital drift and rotational acceleration using: a shape model with axis ratios of 1.94:1.65:1.00, an effective diameter of 1.55 ± 0.07 km, a geometric albedo of 0.20 ± 0.02, a thermal inertia of 140-100+140J m-2K-1s−1/2, a highly rough surface, and a bulk density of 2850-680+480kg m-3. Using these properties we predict that Apollo’s obliquity is increasing towards the 180° YORP asymptotic state at a rate of 1.5-0.5+0.3degrees per 105yr.ConclusionsThe derived thermal inertia suggests that Apollo has loose regolith material resting on its surface, which is consistent with Apollo undergoing a recent resurfacing event based on its observed Q-type spectrum. The inferred bulk density is consistent with those determined for other S-type asteroids, and suggests that Apollo has a fractured interior. The YORP effect is acting on a much faster timescale than the Yarkovsky effect and will dominate Apollo’s long term evolution. The ATPM can readily be applied to other asteroids with similar observational data sets.
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发表时间：
1981
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影响因子：
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DOI：
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发表时间：
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