正列參數：恆星形成區域團塊之碎塊排列的量化

Abstract

作為高質量恆星前身的緻密核，它們通常形成於高密度的團塊中，並在空間上呈現出多樣化的排列。近年觀測產生的大量數據使得有效地量化這些排列顯得日益重要，而此舉也有利於將這些排列與團塊尺度的特性更有系統地連結。故此，我們引入「正列參數」以量化緻密核排列程度，並展現此參數能有效地辨別這些排列。我們將其應用於ASHES計畫的1.3毫米連續譜資料，發現其量化後數值結果符合人眼判別。此外，我們亦利用正列參數尋求其與團塊尺度之特性間的連結。而我們也更進一步地使用數值模擬來探討緻密核排列與更大尺度結構的形成以及團塊演化的關係性。以結果而言，觀測數據及模擬資料僅表明存在弱相關性，這意味著緻密核的排列在團塊演化過程中可能有著動態且局域的特性。

Dense cores, precursors to high-mass stars, form inside the dense clumps and spatially exhibit diverse degrees of alignments. The large data from recent observations necessitate an efficient method to quantify core alignment and systematically relate it to clump-scale properties. Thus, we introduce the alignment parameter to quantify core alignment, and show that it can effectively distinguish between fragmentation modes. We apply it to 1.3 mm dust continuum data from the ASHES survey, demonstrating this parameter is consistent with visual classification. Nevertheless, we conduct correlations between clump-scale parameters and alignment parameters to assess their relation. Also, numerical simulations are used to check for the relation between the core alignment and structure formation, and clump evolution. Both observations and simulations suggest a weak correlation, implying core alignment might be a dynamic and local feature within clump fragmentation.