标题： 光度爆发对原行星盘中岩石颗粒及其冰幔丰度的影响 显示英文标题

标题： The Effect of Luminosity Outbursts on the Abundance of Pebbles and Their Ice Mantles in Protoplanetary Disks

摘要： 厘米大小的尘粒（鹅卵石）对于通过流体不稳定形成星子是必要的，它们在形成行星核心和巨行星以及向其大气层富集化学元素方面发挥着重要作用。 本研究调查了光度爆发对原行星盘中鹅卵石及其冰幔丰度的影响。 我们使用二维流体动力学薄盘FEOSAD代码，对该自引力粘性原行星盘的形成和演化进行了全局模拟，该代码能够自洽地再现光度爆发。 该模型包括热平衡、尘埃演化及其与气体的相互作用、磁流体力学不稳定性的发展、四种挥发性化合物（H$_2$O、CO$_2$、CH$_4$和CO）的吸附和解吸，以及冰幔对尘埃碎裂特性的影响反馈。 我们表明，光度爆发对CO$_2$、CH$_4$和CO雪线的位置影响比水雪线更强。 这是因为H$_2$O雪线在早期盘演化阶段落在粘性加热主导区域，而其他分子的雪线位于恒星辐射加热主导的区域，因此在爆发期间对温度变化更敏感。 尽管如此，由于水分冰的损失导致尘埃聚集体分解为单体，光度爆发使盘中鹅卵石总量减少了一半。 爆发结束后几千年内，由于碰撞凝聚，鹅卵石得以恢复，但恢复时间尺度显著超过水分冻结时间。 冰幔解吸发生在盘中复杂的非轴对称二维区域，在引力不稳定盘早期演化过程中形成螺旋次结构时。 显示英文摘要

摘要： Centimeter-sized dust grains-pebbles-are necessary for planetesimal formation via the streaming instability, they play an important role in forming protoplanetary cores and giant planets, as well as enriching their atmospheres with chemical elements. This work investigates the effect of luminosity outbursts on the abundance of pebbles and their ice mantles in protoplanetary disks. We perform global simulations of formation and evolution of a self-gravitating viscous protoplanetary disk using the 2D hydrodynamic thin-disk FEOSAD code, which self-consistently reproduces luminosity outbursts. The model includes thermal balance, dust evolution and its interaction with gas, development of magnetorotational instability, adsorption and desorption of four volatile compounds (H$_2$O, CO$_2$, CH$_4$ and CO), and the feedback of ice mantles on dust fragmentation properties. We show that luminosity outbursts have a stronger effect on the positions of CO$_2$, CH$_4$ and CO snowlines compared to the water snowline. This is because the H$_2$O snowline falls within the viscous heating dominated region during early disk evolution stages, while snowlines of other molecules are located in regions dominated by stellar irradiation heating and are thus more sensitive to temperature changes during outbursts. Nevertheless, luminosity outbursts reduce the total amount of pebbles in the disk by half due to destruction of dust aggregates into monomers following the loss of water ice that binds the aggregates together. Pebble recovery occurs over several thousand years after the outburst ends due to collisional coagulation, with recovery timescales significantly exceeding water freeze-out times. Ice mantle desorption occurs in a complex non-axisymmetric 2D region of the disk, associated with spiral substructure formation during early evolution of gravitationally unstable disks.