Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 714, Issue 1, Pages L58-L63Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/714/1/L58
Keywords
ISM: clouds; magnetohydrodynamics (MHD); radiative transfer; stars: formation
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Funding
- Ministry of Education, Culture, Sports, Science, and Technology (MEXT) [21244021, 16204012, 20540238, 20740115, 21740136]
- Japan Society for the Promotion of Science (JSPS) for Young Scientists
- Grants-in-Aid for Scientific Research [21244021, 16204012] Funding Source: KAKEN
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We perform a three-dimensional nested-grid radiation magnetohydrodynamics (RMHD) simulation with self-gravity to study the early phase of the low-mass star formation process from a rotating molecular cloud core to a first adiabatic core just before the second collapse begins. Radiation transfer is implemented with the flux-limited diffusion approximation, operator-splitting, and implicit time integrator. In the RMHD simulation, the outer region of the first core attains a higher entropy and its size is larger than that in the magnetohydrodynamics simulations with the barotropic approximation. Bipolar molecular outflow consisting of two components is driven by magnetic Lorentz force via different mechanisms, and shock heating by the outflow is observed. Using the RMHD simulation we can predict and interpret the observed properties of star-forming clouds, first cores, and outflows with millimeter/submillimeter radio interferometers, especially the Atacama Large Millimeter/submillimeter Array.
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