论文标题
超短期的行星TOI-1807B的新参数测量
New Parameter Measurements for the Ultra-Short-Period Planet TOI-1807b
论文作者
论文摘要
Ultra-Short-Period（USP）行星是轨道时期非常短的外部行星（$ \ textit {p} <1美元$ day），而TOI-1807b是Tess Mission最近发现的一个这样的行星，在该行星中，TOI-1807系统中的IT Orbits在TOI-1807系统中仍然鲜为人知。 In this paper, we re-analyzed the transit light curves of TOI-1807 using the latest TESS data from Sector 49, combined with previous data from Sector 22 and 23. By running the MCMC simulation through all three sectors, we found that our transit model fits the data from Sector 49 the best, and we deduced that TOI-1807b is a Super-Earth with a mass of $ 2.27^{+0.49} _ { - 0.58} \，m_ \ oplus $，半径为$ 1.37^{+0.10} _ { - 0.09} \，r_ \ oplus $，密度为$ 0.875^{+0.875^{+0.264} $ 0.264} $ 0.264） $ 1499^{+82} _ { - 129} \，\ mathrm {k} $的表面温度。我们确认TOI-1807b轨道大约$ 0.0135^{+0.0013} _ { - 0.0022} \，\ Mathrm {au} $，周期为$ 0.54929^{+0.00012} {+0.00012} _ _ { - 0.005} _ { - 0.005} \ planiase interipity in Mathisity wisteripy white planise white ant Outeripy white protizity white protisy protizity prounity。由于自旋轨道同步，潮汐锁定。此外，我们建议TOI-1807b可能会慢慢地经历其轨道衰减过程，我们进一步确定TOI-1807b处于圆形的同步轨道，由于潮汐而永久变形，导致$ \ sim $ 4％的密度校正$ 4％。由于TOI-1807是如此年轻的明星，年龄仅为$ 300 \ pm 80 \，\ mathrm {Myr} $，因此我们还暗示，从Active Toi-1807发出的辐射可能是如此强烈，以至于它可能已经破坏了TOI-1807b表面上的大部分大气。
The ultra-short-period (USP) planets are exoplanets with very short orbital periods ($\textit{P} < 1$ day), and TOI-1807b is one such planet recently discovered by the TESS mission where it orbits in the TOI-1807 system that is still little known nowadays. In this paper, we re-analyzed the transit light curves of TOI-1807 using the latest TESS data from Sector 49, combined with previous data from Sector 22 and 23. By running the MCMC simulation through all three sectors, we found that our transit model fits the data from Sector 49 the best, and we deduced that TOI-1807b is a Super-Earth with a mass of $2.27^{+0.49}_{-0.58}\, M_\oplus$, a radius of $1.37^{+0.10}_{-0.09}\, R_\oplus$, a density of $0.875^{+0.264}_{-0.285}\, ρ_\oplus$, and a surface temperature of $1499^{+82}_{-129}\, \mathrm{K}$. We confirmed that TOI-1807b orbits at approximately $0.0135^{+0.0013}_{-0.0022}\, \mathrm{AU}$ with a period of $0.54929^{+0.00012}_{-0.00005}\, \mathrm{days}$, which raises the possibility of the planet being tidally locked due to spin-orbit synchronization. In addition, we suggest that TOI-1807b might slowly undergo its orbital decay process, and we further identify that TOI-1807b is in a circular, synchronous orbit and permanently deformed due to tides, leading to $\sim$4% correction in density. Since TOI-1807 is such a young star with an age of only $300 \pm 80\, \mathrm{Myr}$, we also imply that the radiation emitted from active TOI-1807 could be so intense that it might have destroyed most of the atmosphere over the surface of TOI-1807b.
