论文标题
牛顿后对某些特征性系外行星的特征时间尺度的影响
Post-Newtonian effects on some characteristic timescales of transiting exoplanets
论文作者
论文摘要
Some measurable characteristic timescales $\left\{t_\mathrm{trn}\right\}$ of transiting exoplanets are investigated in order to check preliminarily if their cumulative shifts over the years induced by the post-Newtonian (pN) gravitoelectric (Schwarzschild) and gravitomagnetic (Lense-Thirring) components of the至少在原则上，恒星重力场是可测量的。考虑了主要的（星球前的行星）和次级（星星背后的行星）及其相关的特征时间间隔：总运输持续时间$ t_d $，Ingress/Egress/Egress Transit $τ$，全半宽度，最大最大主要持续时间$ T_H $，以及Conjununtion $ T_ $ t_ \ t_ \ t_ \ t_ cj cj Jj cj J. For each of them, the net changes per orbit $\langleΔt_D\rangle,\,\langleΔτ\rangle,\,\langleΔt_H\rangle,\,\langleΔt_\mathrm{cj}\rangle$ induced by the aforementioned pN accelerations are analytically obtained;还制定了这颗恒星四极质量时刻$ j_2^\ star $的牛顿效应。它们是针对边缘椭圆形轨道中虚拟的太阳jupter系统计算的，结果与HD 286123 B系外行星的当前实验精度进行了比较。它的pn gravitoeleclectric shift $ \ left \langleΔt_\ mathrm {cj}^\ mathrm {1pn} \ right \ rangle $ $可能会在原则上变得可衡量，至少在$ \ simeq 8 \ simeq 8 \ simeq 8 \ simeq 8 \ times 10^{ - 5} $ plucative of（正式）相对级别的相对范围中，大约30年的相对范围，以相对范围30年。例如，诸如造成时间标准，忽略星空，忽视云的混淆的系统学可能会恶化实际准确性。提出的方法足以将其应用于修饰的重力模型。
Some measurable characteristic timescales $\left\{t_\mathrm{trn}\right\}$ of transiting exoplanets are investigated in order to check preliminarily if their cumulative shifts over the years induced by the post-Newtonian (pN) gravitoelectric (Schwarzschild) and gravitomagnetic (Lense-Thirring) components of the stellar gravitational field are, at least in principle, measurable. Both the primary (planet in front of the star) and the secondary (planet behind the star) transits are considered along with their associated characteristic time intervals: the total transit duration $t_D$, the ingress/egress transit duration $τ$, the full width at half maximum primary transit duration $t_H$, and also the time of conjunction $t_\mathrm{cj}$. For each of them, the net changes per orbit $\langleΔt_D\rangle,\,\langleΔτ\rangle,\,\langleΔt_H\rangle,\,\langleΔt_\mathrm{cj}\rangle$ induced by the aforementioned pN accelerations are analytically obtained; also the Newtonian effect of the star's quadrupole mass moment $J_2^\star$ is worked out. They are calculated for a fictitious Sun-Jupiter system in an edge-on elliptical orbit, and the results are compared with the present-day experimental accuracies for the HD 286123 b exoplanet. Its pN gravitoelectric shift $\left\langleΔt_\mathrm{cj}^\mathrm{1pN}\right\rangle$ may become measurable, at least in principle, at a $\simeq 8\times 10^{-5}$ level of (formal) relative accuracy after about 30 years of continuous monitoring corresponding to about 1000 transits. Systematics like, e.g., confusing time standards, neglecting star spots, neglecting clouds, would likely deteriorate the actual accuracy. The method presented is general enough to be applied also to modified models of gravity.
