论文标题
插入位置，早期圆盘尺寸和自我碎片零散光盘的比例之间的联系
The link between infall location, early disc size, and the fraction of self-gravitationally fragmenting discs
论文作者
论文摘要
许多原球盘在生活的早期都是自我磨损的。如果它们在自己的重力下碎裂，它们会形成绑定的气态团块，可能演变为巨型行星。如今，仍未知的圆盘的比例以及可能导致通过重力不稳定性形成巨大行星的条件的频率。 我们执行从形成到分散的圆盘的种群综合。在改变进口半径时，我们研究了早期椎间盘大小与碎片的关系。此外，我们研究了恒星积聚加热如何影响碎片分数。 我们发现，只有碟片在生命的早期就变得足够大时才碎片。这种尺寸敏感地取决于其母体分子云芯的崩溃期间将质量添加到椎间盘中的位置。通过选择与观察到的中间圆盘尺寸分布相一致的合成圆盘尺寸分布的中间位置，我们发现片段化分数在0.1至11％之间，具体取决于圆盘的恒星积聚加热的效率。 我们得出的结论是，早期的椎间盘大小主要取决于分子云核心崩溃期间的插座位置，并控制碎裂的整体频率。恒星积聚加热对于碎裂起着重要作用，必须进一步研究。我们的工作是通过重力不稳定性朝着对巨型行星形成频率进行预测的明智的一步。即将进行的观察和理论研究将加深我们对椎间盘的形成和早期演变的理解，最终使我们了解如何通过引力不稳定和观察到的外星球群联系在一起，并了解如何通过引力不稳定而形成巨型行星。
Many protoplanetary discs are self-gravitating early in their lives. If they fragment under their own gravity, they form bound gaseous clumps which may evolve to become giant planets. Today, the fraction of discs that undergo fragmentation, and the frequency of conditions that may lead to giant planet formation via gravitational instability, is still unknown. We perform a population synthesis of discs from formation to dispersal. In varying the infall radius, we study the relationship of the early disc size with fragmentation. Furthermore, we investigate how stellar accretion heating affects the fragmentation fraction. We find that discs fragment only if they become sufficiently large early in their lives. This size depends sensitively on where mass is added to the discs during the collapse of their parent molecular cloud core. By choosing intermediate infall locations leading to a synthetic disc size distribution that is in agreement with the observed one, we find a fragmentation fraction between 0.1 and 11 %, depending on the efficiency of stellar accretion heating of the discs. We conclude that the early disc size is mainly determined by the infall location during the collapse of the molecular cloud core and controls the population-wide frequency of fragmentation. Stellar accretion heating plays an important role for fragmentation and must be studied further. Our work is an observationally-informed step towards a prediction of the frequency of giant planet formation by gravitational instability. Upcoming observations and theoretical studies will deepen our understanding of the formation and early evolution of discs, eventually allowing to understand how infall, disc morphology, giant planet formation via gravitational instability, and the observed extrasolar planet population are linked.
