Dynamical Formation of Close Binaries during the Pre-main-sequence Phase

Dynamical Formation of Close Binaries during the Pre-main-sequence Phase

Solar-type binaries with short orbital periods (P-close equivalent to 1-10. days; a less than or similar to 0.1. au) cannot form directly via fragmentation of molecular clouds or protostellar disks, yet their component masses are highly correlated, suggesting interaction during the pre-main-sequence...

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Bibliographic Details
Main Authors: Moe, Maxwell, Kratter, Kaitlin M.
Other Authors: Univ Arizona, Steward Observ
Language:en
Published: IOP PUBLISHING LTD 2018
Subjects:
binaries: close
stars: formation
stars: kinematics and dynamics
stars: pre-main sequence
Online Access:http://hdl.handle.net/10150/627100
http://arizona.openrepository.com/arizona/handle/10150/627100

Internet

http://hdl.handle.net/10150/627100
http://arizona.openrepository.com/arizona/handle/10150/627100

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