论文标题
在下一个将来，汞的2pn围栏进攻是否可以衡量？
Might the 2PN perihelion precession of Mercury become measurable in the next future?
论文作者
论文摘要
Hermean的平均圆锥体率$ \dotΩ^\ mathrm {2pn} $，计算到第二个牛顿后（2pn）订单，带有高斯扰动方程式和示波的keplerian轨道元素，范围从$ -18 $ -4 $ -4 $ -4 $ -4 $ $ -4 $ $ -4 $ $ -4 $ $ -4 $ microarcsecondss $ \ left（μ\ mathrm {as \，cty}^{ - 1} \ right）$，具体取决于epoch $ f_0 $的真正异常。这是四个贡献的总和：其中之一是进入运动方程的2PN加速度的直接结果，而其他三个是太阳重力场的1PN分量的间接效应。对实验汞的围栏率$ \dotΩ_\ Mathrm {Exp} $的正式不确定性的评估，本本作者最近发表的，基于Astronomers E.V. EPM2017 Planetary Esphemerides的51年Radiotechnical数据。 Pitjeva和N.P. pitjev，为$σ_{\dotΩ_\ Mathrm {exp}} \ simeq 8 \，μ\ mathrm {as \，cty}^{ - 1} $，对应于相对准确性$ 2 \ $ 2 \ times 10^{ - 7} $的相对准确性$ 2 { - 7n} $ $ \ eft $ \ eft $ \ eft（ $β$和$γ$缩放众所周知的1pn围栏序列。实际上，尽管重新处理了以前Messenger任务的现有原始数据，但现实的不确定性可能会高达$ \ simeq 10-50 $倍，并且最近改进的太阳能电晕模型应该可以改善我们对HERMEAN ORBIT的了解。目前前往汞的贝皮科洛姆海上航天器可能会达到$ \ simeq 10^{ - 7} $在约束$β$和$γ$的准确性水平上，尽管$ \ simeq 10^{ - 6} $看起来根据目前可用于文献中的大多数模拟。因此，在不久的将来，也可能有必要在太阳系的动力学中加速2PN加速。
The Hermean average perihelion rate $\dotω^\mathrm{2PN}$, calculated to the second post-Newtonian (2PN) order with the Gauss perturbing equations and the osculating Keplerian orbital elements, ranges from $-18$ to $-4$ microarcseconds per century $\left(μ\mathrm{as\,cty}^{-1}\right)$, depending on the true anomaly at epoch $f_0$. It is the sum of four contributions: one of them is the direct consequence of the 2PN acceleration entering the equations of motion, while the other three are indirect effects of the 1PN component of the Sun's gravitational field. An evaluation of the merely formal uncertainty of the experimental Mercury's perihelion rate $\dotω_\mathrm{exp}$ recently published by the present author, based on 51 years of radiotechnical data processed with the EPM2017 planetary ephemerides by the astronomers E.V. Pitjeva and N.P. Pitjev, is $σ_{\dotω_\mathrm{exp}}\simeq 8\,μ\mathrm{as\,cty}^{-1}$, corresponding to a relative accuracy of $2\times 10^{-7}$ for the combination $\left(2 + 2γ- β\right)/3$ of the PPN parameters $β$ and $γ$ scaling the well known 1PN perihelion precession. In fact, the realistic uncertainty may be up to $\simeq 10-50$ times larger, despite reprocessing the now available raw data of the former MESSENGER mission with a recent improved solar corona model should ameliorate our knowledge of the Hermean orbit. The BepiColombo spacecraft, currently en route to Mercury, might reach a $\simeq 10^{-7}$ accuracy level in constraining $β$ and $γ$ in an extended mission, despite $\simeq 10^{-6}$ seems more likely according to most of the simulations currently available in the literature. Thus, it might be that in the not too distant future it will be necessary to include the 2PN acceleration in the Solar System's dynamics as well.
