Abstract
We use the properties of OB runaway stars and, assuming that they are ejected from their parent clusters by dynamical binary-binary interactions, deduce certain necessary characteristics of high-mass star formation. We deduce that massive stars form in small groups of binaries that are biased towards unit mass ratio, and that within these groups the IMF is severely under-represented in low-mass stars compared with the field star IMF
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
