发表机构
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文综述ALMA问世10年来原行星盘引力不稳定性的理论与观测进展，揭示其从巨行星形成理论机制转变为可通过高分辨率观测检验的丰富物理框架。
AI 中文摘要
在恒星与行星形成的最初阶段，年轻恒星周围的原行星盘可能会变得引力不稳定。若原行星盘质量足够大，其自引力会触发大尺度旋臂的形成，旋臂可传输角动量、捕获固体颗粒，还可能坍缩形成亚恒星伴星。本文综述了自ALMA问世以来10年间原行星盘引力不稳定性研究的理论与观测进展，这些进展改变了人类对引力不稳定性的认知，使其从过去作为巨行星形成的理论机制，转变为可通过高分辨率观测直接检验的物理内涵丰富的框架。
英文摘要
During the earliest phases of star and planet formation, a young star is surrounded by a disc that can become gravitationally unstable. Indeed, if the protoplanetary disc is sufficiently massive, its self-gravity triggers the formation of large scale spiral arms, transporting angular momentum, trapping solid particles and, potentially, collapsing to form sub-stellar companions. In this paper, we review the theoretical and observational advances in the study of gravitational instability in protoplanetary discs over the last 10 years, since the advent of ALMA. These developments have transformed our understanding of gravitational instability, moving beyond its historical role as a theoretical mechanism for giant planet formation toward a physically rich framework that can be directly tested against high-resolution observations.
CommentsPublished on Frontiers in Astronomy and Space Sciences - Planetary Science, special issue: Birthplaces of Planets in Their Earliest Stages: Towards Characterization of Young Protostellar Disks
Journal refVolume 13 - 2026
DOI：10.3389/fspas.2026.1911058
