论文标题
在太阳能社区中的年轻星星的运动学炎热人数
A kinematically hot population of young stars in the solar neighbourhood
论文作者
论文摘要
在过去的三十年中，已经确定了附近的几百名年轻恒星移动组（MG）成员，但是有少量化或表征不属于先前确定的MGS的年轻恒星的系统努力较少。我们发现，在100 pc内使用运动学上的225颗富含锂的恒星的样品，我们发现只有$ 50 \ pm 10 $ 10 $的年轻人（$ \ \ lyseSim 125 $ Myr），低质量（$ 0.5 <m/m _ {\ odot} <1.0 $）星星与已知MGS相关。虽然我们发现一些证据表明，六个非MG恒星可能与下半人马座的关联有关，其余的在运动学上形成了“更热”的人群，在速度上更广泛地分散，并且在空间中没有明显的浓度。 MG成员和非MG恒星的质量分布相似，但非MG恒星平均可能更老。我们简要讨论了有关非MG人群起源的一些解释。
In the last three decades several hundred nearby members of young stellar moving groups (MGs) have been identified, but there has been less systematic effort to quantify or characterise young stars that do not belong to previously identified MGs. Using a kinematically unbiased sample of 225 lithium-rich stars within 100 pc, we find that only $50 \pm 10$ per cent of young ($\lesssim 125$ Myr), low-mass ($0.5<M/M_{\odot}<1.0$) stars, are kinematically associated with known MGs. Whilst we find some evidence that six of the non-MG stars may be connected with the Lower Centaurus-Crux association, the rest form a kinematically "hotter" population, much more broadly dispersed in velocity, and with no obvious concentrations in space. The mass distributions of the MG members and non-MG stars is similar, but the non-MG stars may be older on average. We briefly discuss several explanations for the origin of the non-MG population.
