Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 897, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8213/ab9d86
Keywords
Multiple star evolution; Star formation; Jets; Magnetic fields; Stellar jets
Categories
Funding
- HPCI System Research Project [hp180001, hp190035, hp200004]
- JSPS KAKENHI [JP17K05387, JP17H02869, JP17H06360, 17KK0096]
- Grants-in-Aid for Scientific Research [17KK0096] Funding Source: KAKEN
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The formation of a close binary system is investigated using a three-dimensional resistive magnetohydrodynamic simulation. Starting from a prestellar cloud, the cloud evolution is calculated until similar to 400 yr after protostar formation. Fragmentation occurs in the gravitationally collapsing cloud, and two fragments evolve into protostars. The protostars orbit each other and a protobinary system appears. A wide-angle low-velocity outflow emerges from the circumbinary streams that enclose two protostars, while each protostar episodically drives high-velocity jets. Thus, the two high-velocity jets are surrounded by the low-velocity circumbinary outflow. The speed of the jets exceeds greater than or similar to 100 km s(-1). Although the jets have a collimated structure, they are swung back on the small scale and are tangled at the large scale due to the binary orbital motion. A circumstellar disk also appears around each protostar. In the early main accretion phase, the binary orbit is complicated, while the binary separation is within <30 au. For the first time, all the characteristics of protobinary systems recently observed with large telescopes are reproduced in a numerical simulation.
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