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dc.contributor.authorLee, Aaron T.
dc.contributor.authorOffner, Stella S. R.
dc.contributor.authorKratter, Kaitlin M.
dc.contributor.authorSmullen, Rachel A.
dc.contributor.authorLi, Pak Shing
dc.date.accessioned2020-02-04T19:41:21Z
dc.date.available2020-02-04T19:41:21Z
dc.date.issued2019-12-23
dc.identifier.citationAaron T. Lee et al 2019 ApJ 887 232en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab584b
dc.identifier.urihttp://hdl.handle.net/10150/636907
dc.description.abstractStars rarely form in isolation. Nearly half of the stars in the Milky Way have a companion, and this fraction increases in star-forming regions. However, why some dense cores and filaments form bound pairs while others form single stars remains unclear. We present a set of three-dimensional, gravo-magnetohydrodynamic simulations of turbulent star-forming clouds, aimed at understanding the formation and evolution of multiple-star systems formed through large-scale (greater than or similar to 10(3) au) turbulent fragmentation. We investigate three global magnetic field strengths, with global mass-to-flux ratios of mu(phi) = 2, 8, and 32. The initial separations of protostars in multiples depend on the global magnetic field strength, with stronger magnetic fields (e.g., mu(phi)= 2) suppressing fragmentation on smaller scales. The overall multiplicity fraction (MF) is between 0.4 and 0.6 for our strong and intermediate magnetic field strengths, which is in agreement with observations. The weak field case has a lower fraction. The MF is relatively constant throughout the simulations, even though stellar densities increase as collapse continues. While the MF rarely exceeds 60% in all three simulations, over 80% of all protostars are part of a binary system at some point. We additionally find that the distribution of binary spin misalignment angles is consistent with a randomized distribution. In all three simulations, several binaries originate with wide separations and dynamically evolve to less than or similar to 10(2) au separations. We show that a simple model of mass accretion and dynamical friction with the gas can explain this orbital evolution.en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://iopscience.iop.org/info/page/text-and-data-mining
dc.titleThe Formation and Evolution of Wide-orbit Stellar Multiples In Magnetized Cloudsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume887
dc.source.issue2
dc.source.beginpage232
refterms.dateFOA2020-02-04T19:41:22Z


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