NGC 2264星系团的吸积和盘诊断研究
A study of accretion and disk diagnostics in the NGC 2264 cluster
摘要：
了解盘耗散对于研究行星如何形成至关重要。根据金牛T星（TTS）的红外观测结果推断，金牛T星的盘隙和盘洞几乎对应于无尘区，表明存在厚吸积盘和碎片盘之间的过渡阶段。过渡盘通常被认为是新形成行星的候选者。我们搜寻了属于NGC 2264的过渡盘候选者。我们的特点吸积，磁盘，过渡盘候选人的恒星性质，并将它们与系统的完整磁盘和无盘的恒星我们建模的光谱能量分布（SED）的样本的401 TTS，使用光度数据从U波段的MIPS波段的EXTRASED拟合代码。我们使用SED模型来区分过渡盘候选者，完整的磁盘系统和无盘恒星。我们将样本中的$52\%$分类为全盘系统，将$41\%$分类为无盘星，将其中的$7\%$分类为过渡盘候选星，其中7个系统是属于NGC 2264星团的新的过渡盘候选星。根据$α_{IRAC}$分类，过渡盘候选者的样本在内部盘中呈现类似于贫血盘的尘埃，这表明贫血盘系统可以是候选过渡盘。我们发现，在内部磁盘中的尘埃孔的存在下，并没有停止吸积过程，因为过渡盘候选人的$82\%$吸积和显示$Hα$，紫外线过剩，并在同一水平的完整的磁盘系统的质量吸积率。我们估计的内孔大小，从0.1到$78AU$，过渡盘候选人的样本。只有$18\%$的过渡盘候选者，洞的大小可以解释的X射线光蒸发恒星辐射。
英文摘要：
Understanding disk dissipation is essential for studying how planets form. Disk gaps and holes, which almost correspond to dust-free regions, are inferred from infrared observations of T Tauri stars (TTS), indicating the existence of a transitional phase between thick accreting disks and debris disks. Transition disks are usually referred to as candidates for newly formed planets. We searched for transition disk candidates belonging to NGC 2264. We characterized accretion, disk, and stellar properties of transition disk candidates and compared them to systems with a full disk and diskless stars We modeled the spectral energy distribution (SED) of a sample of 401 TTS, with Hyperion SED fitting code using photometric data from the U band to the MIPS band. We used the SED modeling to distinguish transition disk candidates, full disk systems, and diskless stars. We classified $52\%$ of the sample as full disk systems, $41\%$ as diskless stars, and $7\%$ of the systems as transition disk candidates, among which seven systems are new transition disk candidates belonging to the NGC 2264 cluster. The sample of transition disk candidates present dust in the inner disk similar to anemic disks, according to the $α_{IRAC}$ classification, which shows that anemic disk systems can be candidate transition disks. We show that the presence of a dust hole in the inner disk does not stop the accretion process since $82\%$ of transition disk candidates accrete and show $Hα$, UV excess, and mass accretion rates at the same level as full disk systems. We estimate the inner hole sizes, ranging from 0.1 to $78AU$, for the sample of transition disk candidates. In only $18\%$ of the transition disk candidates, the hole size could be explained by X-ray photoevaporation from stellar radiation.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
