论文标题
HD 28109拥有三个传输的Neptunian行星，其中包括一对近共振对，由南极洲的Astep确认
HD 28109 hosts a trio of transiting Neptunian planets including a near-resonant pair, confirmed by ASTEP from Antarctica
论文作者
论文摘要
我们报告了绕着F8 Star HD〜28109的三个行星的发现和表征，该行星位于\ Tess的连续观看区域中。这两个外行星的期限为$ \ rm 56.0067 \ pm 0.0003〜天$和$ \ rm 84.2597 _ { - 0.0008}^{+0.0010}〜天$，这意味着一个周期比非常接近第一个平均运动次数3：2均值的运动量，激动人心的时间恢复到$ night termit termit termit unting unting unting up term unting up unting up unting up unting up $ $ $ $ 60 \，分钟$。这两个行星首先是由\ tess识别的，我们在\ textcolor {black} {\ tess光度法}中确定了第三个行星，其周期为$ \ rm 22.8911 \ pm 0.0004〜天$。我们使用Hazelwood，ASTEP和LCO的地面光度法确认了所有三个行星候选者的行星性质，包括对$ \ rm \ sim9 \，H $ hd $ transit的HD〜28109 c的H $ Transit完全检测。这三个行星的半径是\ textColor {black} {$ \ rm r_b = 2.199 _ { - 0.10}^{+0.098} 〜r _ {\ oplus} $，$ \ rm r_c = 4.23 r_d = 3.25 \ pm0.11〜r _ {\ oplus} $};我们使用ttvs和浓咖啡和竖琴的精确径向速度来表征它们的质量，并发现它们为$ \ rm m_b = 18.5 _ { - 7.6}^{+9.1} 〜m _ {\ oplus} $，$ \ rm \ rm \ rm \ rm M_c=7.9_{-3.0}^{+4.2}~M_{\oplus}$ and $\rm M_d=5.7_{-2.1}^{+2.7}~M_{\oplus}$, making planet b a dense, massive planet while c and d are both under-dense.我们还证明了这两个外行星使用传输光谱术在大气表征上成熟，尤其是考虑到它们在JWST的CVZ中的位置。迄今为止获得的数据与共振（库）和非谐振（循环）解决方案一致；其他观察结果将表明这对夫妇实际上是锁定在共振中还是几乎恢复。
We report on the discovery and characterisation of three planets orbiting the F8 star HD~28109, which sits comfortably in \tess's continuous viewing zone. The two outer planets have periods of $\rm 56.0067 \pm 0.0003~days$ and $\rm 84.2597_{-0.0008}^{+0.0010}~days$, which implies a period ratio very close to that of the first-order 3:2 mean motion resonance, exciting transit timing variations (TTVs) of up to $\rm 60\,mins$. These two planets were first identified by \tess, and we identified a third planet in the \textcolor{black}{\tess photometry} with a period of $\rm 22.8911 \pm 0.0004~days$. We confirm the planetary nature of all three planetary candidates using ground-based photometry from Hazelwood, ASTEP and LCO, including a full detection of the $\rm \sim9\,h$ transit of HD~28109 c from Antarctica. The radii of the three planets are \textcolor{black}{$\rm R_b=2.199_{-0.10}^{+0.098} ~R_{\oplus}$, $\rm R_c=4.23\pm0.11~ R_{\oplus}$ and $\rm R_d=3.25\pm0.11 ~R_{\oplus}$}; we characterise their masses using TTVs and precise radial velocities from ESPRESSO and HARPS, and find them to be $\rm M_b=18.5_{-7.6}^{+9.1}~M_{\oplus}$, $\rm M_c=7.9_{-3.0}^{+4.2}~M_{\oplus}$ and $\rm M_d=5.7_{-2.1}^{+2.7}~M_{\oplus}$, making planet b a dense, massive planet while c and d are both under-dense. We also demonstrate that the two outer planets are ripe for atmospheric characterisation using transmission spectroscopy, especially given their position in the CVZ of JWST. The data obtained to date are consistent with resonant (librating) and non-resonant (circulating) solutions; additional observations will show whether the pair is actually locked in resonance or just near-resonant.
