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    The Formation and Evolution of Wide-orbit Stellar Multiples In Magnetized Clouds

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    Lee_2019_ApJ_887_232.pdf
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    Author
    Lee, Aaron T.
    Offner, Stella S. R.
    Kratter, Kaitlin M.
    Smullen, Rachel A.
    Li, Pak Shing
    Affiliation
    Univ Arizona, Dept Astron
    Issue Date
    2019-12-23
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Aaron T. Lee et al 2019 ApJ 887 232
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    Copyright © 2019. The American Astronomical Society. All rights reserved.
    Collection Information
    This 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.
    Abstract
    Stars 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.
    ISSN
    0004-637X
    DOI
    10.3847/1538-4357/ab584b
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab584b
    Scopus Count
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    UA Faculty Publications

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