ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): How Do Dense Core Properties Affect the Multiplicity of Protostars?

During the transition phase from a prestellar to a protostellar cloud core, one or several protostars can form within a single gas core. The detailed physical processes of this transition, however, remain unclear. We present 1.3 mm dust continuum and molecular line observations with the Atacama Larg...

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Detalles Bibliográficos
Autores: Dutta, Somnath, Lee, Chin-Fei, Hirano, Naomi, Liu, Tie, Johnstone, Doug, Liu, Sheng-Yuan, Tatematsu, Ken'ichi, Goldsmith, Paul F., Sahu, Dipen, Evans, Neal D., Sanhueza, Patricio, Kwon, Woojin, Qin, Sheng-Li, Ranjan Samal, Manash, Zhang, Qizhou, Kim, Kee-Tae, Shang, Hsien, Lee, Chang Won, Moraghan, Anthony, Jhan, Kai-Syun, Li, Shanghuo, Lee, Jeong-Eun, Traficante, A., Juvela, Mika, Bronfman, L., Eden, David J., Soam, Archana, He, Jinhua, Yi, Hee-Weon, Liu, Hong-li, Kuan, Yi-Jehng, Pelkonen, Veli Matti, Luo, Qiuyi, Hsu, Shih-Ying
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/279658
Acceso en línea:http://hdl.handle.net/10261/279658
Access Level:acceso abierto
Palabra clave:Star formation
Low mass stars
Stellar jets
Stellar winds
Protostars
Astrochemistry
Stellar mass loss
Stellar evolution
Young stellar objects
Early stellar evolution
Descripción
Sumario:During the transition phase from a prestellar to a protostellar cloud core, one or several protostars can form within a single gas core. The detailed physical processes of this transition, however, remain unclear. We present 1.3 mm dust continuum and molecular line observations with the Atacama Large Millimeter/submillimeter Array toward 43 protostellar cores in the Orion molecular cloud complex (λ Orionis, Orion B, and Orion A) with an angular resolution of ∼0.″35 (∼140 au). In total, we detect 13 binary/multiple systems. We derive an overall multiplicity frequency (MF) of 28% ± 4% and a companion star fraction (CSF) of 51% ± 6%, over a separation range of 300-8900 au. The median separation of companions is about 2100 au. The occurrence of stellar multiplicity may depend on the physical characteristics of the dense cores. Notably, those containing binary/multiple systems tend to show a higher gas density and Mach number than cores forming single stars. The integral-shaped filament of the Orion A giant molecular cloud (GMC), which has the highest gas density and hosts high-mass star formation in its central region (the Orion Nebula cluster), shows the highest MF and CSF among the Orion GMCs. In contrast, the λ Orionis GMC has a lower MF and CSF than the Orion B and Orion A GMCs, indicating that feedback from H ii regions may suppress the formation of multiple systems. We also find that the protostars comprising a binary/multiple system are usually at different evolutionary stages.

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