From the 1 of 14 linked papers with an AI index.
14 papers
How Should We Understand the Core Mass Function? A memo of the CMF2IMF conference at ESO Garching
Fengwei Xu, Roberto Galvan-Madrid, Kaho Morii +4
The paper reviews efforts to link the core mass function (CMF) to the stellar initial mass function (IMF), compiles observational core catalogs into a common framework via the publ…
The dominance of turbulence over magnetism in the formation of massive star cluster seeds
Junhao Liu, Patricio Sanhueza, Piyali Saha +32
High-mass stars form in protoclusters, where gravo-magnetic processes shape collapsing clouds and clumps to be elongated preferentially perpendicular to magnetic (B) fields. Yet it…
Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 m Dark Massive Clumps
Kaho Morii, Patricio Sanhueza, Qizhou Zhang +1
Gravitational collapse is fundamental to star formation, yet direct kinematic evidence of infall at the core scale in high-mass star-forming regions remains poorly constrained. We…
Digging into the Interior of Hot Cores with ALMA (DIHCA). VI. The Formation of Low-mass Multiple Systems in High-mass Cluster-forming Regions
Qiuyi Luo, Patricio Sanhueza, Stella S. R. Offner +14
Most stars form in multiple systems, with profound implications in numerous astronomical phenomena intrinsically linked to multiplicity. However, our knowledge about the process on…
Digging into the Interior of Hot Cores with ALMA (DIHCA). VII. Disk candidates around high-mass stars and evidence of anisotropic infall
Fernando A. Olguin, Patricio Sanhueza, Yoko Oya +19
We study the kinematics of condensations in 30 fields forming high-mass stars with ALMA at a high-resolution of ~0.08'' on average (~230 au). The presence of disks is important for…
The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). XIII. Core Mass Function, Lifetime, and Growth of Prestellar Cores
Kaho Morii, Patricio Sanhueza, Qizhou Zhang +10
The core mass function (CMF) of prestellar cores is essential for understanding the initial conditions of star and cluster formation. However, the universality of the CMF and its r…