| الوصف: |
Star formation takes place in dense cores within molecular clouds. These cores are characterised by higher densities and lower temperatures compared to the parental cloud (Caselli et al., 2002). Observations using high-density (>104 cm-3) tracers show the turbulence inside dense cores to be subsonic (Barranco & Goodman, 1998), in contrast to the supersonic turbulence in the large-scale ambient cloud (Larson, 1981). Understanding the transition from the cloud to subsonic dense cores is imperative in the study of core formation, as the dissipation of turbulence is an essential step in the process. This transition region could also help understand the connection between the cores and the ambient molecular cloud. NH3 inversion transitions are ideal tracers to observe the dense cores and surrounding cloud, which have inherently different densities (Choudhury et al., 2021). The subsonic dense cores are usually thought to be well- separated from their natal cloud, and evolve as isolated units. However, it has not been studied with high sensitivity in the vicinity of the cores to study whether the cores indeed share a sharp boundary with the surrounding cloud, or there are structures connecting the cores to the cloud. The later scenario would imply that further accretion of material might be possible onto the core, which changes our understanding of the morphology and the dynamical evolution of dense cores. In this poster,we present some of the results from our recent study in L1688 addressing these questions. |
