期刊
ASTROPHYSICAL JOURNAL
卷 791, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/791/1/43
关键词
ISM: clouds; ISM: individual objects (Lupus I); ISM: magnetic fields; polarization; submillimeter: ISM
资金
- NASA [NAG5-12785, NAG5-13301, NNGO-6GI11G, NNX0-9AB98G]
- Illinois Space Grant Consortium)
- Canadian Space Agency (CSA)
- Leverhulme Trust through the Research Project Grant [F/00 407/BN]
- Canadas Natural Sciences and Engineering Research Council (NSERC)
- Canada Foundation for Innovation
- Ontario Innovation Trust
- Puerto Rico Space Grant Consortium
- Fondo Institucional para la Investigacion of the University of Puerto Rico
- National Science Foundation Office of Polar Programs
- Canadian Institute forAdvanced Research
- Spanish Ministry of Economy and Competitiveness (MINECO) [CSD2010-00064]
- STFC [ST/K000926/1, ST/K002023/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K002023/1] Funding Source: researchfish
Turbulence and magnetic fields are expected to be important for regulatingmolecular cloud formation and evolution. However, their effects on sub-parsec to 100 parsec scales, leading to the formation of starless cores, are not well understood. We investigate the prestellar core structuremorphologies obtained from analysis of the Herschel-SPIRE 350 mu m maps of the Lupus I cloud. This distribution is first compared on a statistical basis to the large-scale shape of the main filament. We find the distribution of the elongation position angle of the cores to be consistent with a random distribution, which means no specific orientation of the morphology of the cores is observed with respect to the mean orientation of the large-scale filament in Lupus I, nor relative to a large-scale bent filament model. This distribution is also compared to the mean orientation of the large-scale magnetic fields probed at 350 mu m with the Balloon-borne Large Aperture Telescope for Polarimetry during its 2010 campaign. Here again we do not find any correlation between the core morphology distribution and the average orientation of the magnetic fields on parsec scales. Our main conclusion is that the local filament dynamics-including secondary filaments that often run orthogonally to the primary filament-and possibly small-scale variations in the local magnetic field direction, could be the dominant factors for explaining the final orientation of each core.
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