论文标题
次纳在40 pc的年轻田野恒星高清18599
A sub-Neptune transiting the young field star HD 18599 at 40 pc
论文作者
论文摘要
绕着附近恒星的年轻恒星旋转的跨球星是测试行星形成和进化理论的理想实验室。但是，迄今为止，只有少数恒星<1年龄<1 Gyr可以容纳过境的系外行星。在这里，我们介绍了HD 18599（300 Myr），附近（d = 40 poc）K Star围绕HD的发现和验证。我们使用Tess，Spitzer和Gaia任务，IRSF，LCO，LCO，PEST和NGTS，GEMINI的Speckle Imageing，Chiron，NRES，Feros和Minerva-Australis的Spectroscopy，使用Tess，Spitzer和Gaia任务的数据来验证候选候选行星。行星的轨道周期为4.13 d，半径为2.7正确。 RV数据产生的3--质量上限为30.5mearth，这是由大型伴侣或典型的年轻恒星的大型观察到的大抖动来解释的。宿主星（V〜9 mag）的亮度使其有利于通过多普勒质量测量值进行详细表征，这将为年轻行星的内部结构提供罕见的视野。
Transiting exoplanets orbiting young nearby stars are ideal laboratories for testing theories of planet formation and evolution. However, to date only a handful of stars with age <1 Gyr have been found to host transiting exoplanets. Here we present the discovery and validation of a sub-Neptune around HD 18599, a young (300 Myr), nearby (d=40 pc) K star. We validate the transiting planet candidate as a bona fide planet using data from the TESS, Spitzer, and Gaia missions, ground-based photometry from IRSF, LCO, PEST, and NGTS, speckle imaging from Gemini, and spectroscopy from CHIRON, NRES, FEROS, and Minerva-Australis. The planet has an orbital period of 4.13 d, and a radius of 2.7Rearth. The RV data yields a 3-sigma mass upper limit of 30.5Mearth which is explained by either a massive companion or the large observed jitter typical for a young star. The brightness of the host star (V~9 mag) makes it conducive to detailed characterization via Doppler mass measurement which will provide a rare view into the interior structure of young planets.
