近地小行星(2100) Ra-Shalom、(3103) Eger、(12711) Tukmit与(161989) Cacus的改进模型
Improved models for near-Earth asteroids (2100) Ra-Shalom, (3103) Eger, (12711) Tukmit & (161989) Cacus
AI总结：
本研究获取4颗近地小行星的新密集光变曲线，结合档案数据通过光变曲线反演得到更精准的形状与自转参数，发现Ra-Shalom可能受YORP加速度影响，并首次给出Tukmit的形状与自转参数。
摘要：
我们呈现了近地小行星(3103) Eger、(161989) Cacus、(2100) Ra-Shalom和(12711) Tukmit的24条新的密集光变曲线，这些数据是2021至2022年间，在“visible NEAs observations survey（可见近地小行星观测巡天）”与“NEO Rapid Observation, Characterization and Key Simulations（近地天体快速观测、表征与关键模拟）”项目框架下，利用西班牙特内里费岛泰德天文台的加那利天体物理研究所80厘米望远镜和Telescopio Abierto Remoto 2望远镜获取的。我们将新数据与档案数据结合，通过光变曲线反演方法计算得到了这些小行星的形状模型和自转状态参数（$P$、$λ$、$β$）。对于(3013) Eger和(161989) Cacus，我们得到的形状模型与自转状态参数和此前研究结果一致，但不确定性更小。对于(2100) Ra-Shalom，我们的结果也与既往研究相符；此外我们发现，大小为$\u03c5 = (0.223\pm0.237)\times10^{-8}$ rad d$^{-2}$的Yarkovsky-O'Keefe-Radzievskii-Paddack加速度能略微提升光变曲线的拟合效果，表明(2100) Ra-Shalom可能受到该加速度的影响。我们还首次给出了(12711) Tukmit的形状模型及其自转状态参数（$P=3.484900 \pm 0.000031$ hr，$λ= 27^{\circ}\pm 8^{\circ}$，$β= 9^{\circ} \pm 15^{\circ}$）。
英文摘要：
We present 24 new dense lightcurves of the near-Earth asteroids (3103) Eger, (161989) Cacus, (2100) Ra-Shalom and (12711) Tukmit, obtained with the Instituto Astrofísico Canarias 80 and Telescopio Abierto Remoto 2 telescopes at the Teide Observatory (Tenerife, Spain) during 2021 and 2022, in the framework of projects visible NEAs observations survey and NEO Rapid Observation, Characterization and Key Simulations. The shape models and rotation state parameters ($P$, $λ$, $β$) were computed by applying the lightcurve inversion method to the new data altogether with the archival data. For (3013) Eger and (161989) Cacus, our shape models and rotation state parameters agree with previous works, though they have smaller uncertainties. For (2100) Ra-Shalom, our results also agree with previous studies. Still, we find that a Yarkovsky - O'Keefe - Radzievskii - Paddack acceleration of $\upsilon = (0.223\pm0.237)\times10^{-8}$ rad d$^{-2}$ slightly improves the fit of the lightcurves, suggesting that (2100) Ra-Shalom could be affected by this acceleration. We also present for the first time a shape model for (12711) Tukmit, along with its rotation state parameters ($P=3.484900 \pm 0.000031$ hr, $λ= 27^{\circ}\pm 8^{\circ}$, $β= 9^{\circ} \pm 15^{\circ}$).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
