2020/09/30 by Shanghuo Li, Patricio Sanhueza, Qizhou Zhang +20
Chemistry · Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxy #Millimeter #Molecular Spectroscopy and Structure #Outflow #Physics #Protostar #Star formation #Stellar, planetary, and galactic studies #Submillimeter Array #astro-ph.GA
paper · pdf · doi:10.3847/1538-4357/abb81f
32 pages, 9 figures, 4 tables, accepted for publication in ApJ
openalex created_date 2020/09/21 · arxiv created 2020/10/29 · openalex publication_date 2020/11/01 · arxiv updated 2020/11/18 · openalex updated_date 2026/08/06
Abstract We present a study of outflows at extremely early stages of high-mass star formation obtained from the ALMA Survey of 70 μ m dark High-mass clumps in Early Stages (ASHES). Twelve massive 3.6−70 μ m dark prestellar clump candidates were observed with the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6. Forty-three outflows are identified toward 41 out of 301 dense cores using the CO and SiO emission lines, yielding a detection rate of 14%. We discover six episodic molecular outflows associated with low- to high-mass cores, indicating that episodic outflows (and therefore episodic accretion) begin at extremely early stages of protostellar evolution for a range of core masses. The time span between consecutive ejection events is much smaller than those found in more evolved stages, which indicates that the ejection episodicity timescale is likely not constant over time. The estimated outflow dynamical timescale appears to increase with core masses, which likely indicates that more massive cores have longer accretion timescales than less massive cores. The lower accretion rates in these 70 μ m dark objects compared to the more evolved protostars indicate that the accretion rates increase with time. The total outflow energy rate is smaller than the turbulent energy dissipation rate, which suggests that outflow-induced turbulence cannot sustain the internal clump turbulence at the current epoch. We often detect thermal SiO emission within these 70 μ m dark clumps that is unrelated to CO outflows. This SiO emission could be produced by collisions, intersection flows, undetected protostars, or other motions.