A Caltech Library Service

Effects of the environment on the multiplicity properties of stars in the STARFORGE simulations

Guszejnov, Dávid and Raju, Aman N. and Offner, Stella S. R. and Grudić, Michael Y. and Faucher-Giguère, Claude-André and Hopkins, Philip F. and Rosen, Anna L. (2022) Effects of the environment on the multiplicity properties of stars in the STARFORGE simulations. . (Unpublished)

[img] PDF - Submitted Version
See Usage Policy.


Use this Persistent URL to link to this item:


Most observed stars are part of a multiple star system, but the formation of such systems and the role of environment and various physical processes is still poorly understood. We present a suite of radiation-magnetohydrodynamic simulations of star-forming molecular clouds from the STARFORGE project that include stellar feedback with varied initial surface density, magnetic fields, level of turbulence, metallicity, interstellar radiation field, simulation geometry and turbulent driving. In our fiducial cloud the raw simulation data reproduces the observed multiplicity fractions for Solar-type and higher mass stars, similar to previous works. However, after correcting for observational incompleteness the simulation under-predicts these values. The discrepancy is likely due to the lack of disk fragmentation, as the simulation only resolves multiples that form either through capture or core fragmentation. The raw mass distribution of companions is consistent with randomly drawing from the initial mass function for the companions of > 1 M_⊙ stars, however, accounting for observational incompleteness produces a flatter distribution similar to observations. We show that stellar multiplicity changes as the cloud evolves and anti-correlates with stellar density. This relationship also explains most multiplicity variations between runs, i.e., variations in the initial conditions that increase stellar density (increased surface density, reduced turbulence) decrease multiplicity. While other parameters, such as metallicity, interstellar radiation, and geometry significantly affect the star formation history or the IMF, varying them produces no clear trend in stellar multiplicity properties.

Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription Paper ItemGIZMO code ItemJournal Article
Guszejnov, Dávid0000-0001-5541-3150
Offner, Stella S. R.0000-0003-1252-9916
Grudić, Michael Y.0000-0002-1655-5604
Faucher-Giguère, Claude-André0000-0002-4900-6628
Hopkins, Philip F.0000-0003-3729-1684
Rosen, Anna L.0000-0003-4423-0660
Additional Information:DG is supported by the Harlan J. Smith McDonald Observatory Postdoctoral Fellowship and the Cottrell Fellowships Award (#27982) from the Research Corporation for Science Advancement. Support for MYG was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51479 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Support for PFH was provided by NSF Collaborative Research Grants 1715847 & 1911233, NSF CAREER grant 1455342, and NASA grants 80NSSC18K0562 & JPL 1589742. SSRO and ANR are supported by NSF Career Award AST-1748571 and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. CAFG was supported by NSF through grants AST-1715216, AST-2108230, and CAREER award AST-1652522; by NASA through grant 17-ATP17-0067; by STScI through grant HST-AR-16124.001-A; and by the Research Corporation for Science Advancement through a Cottrell Scholar Award. ALR acknowledges support from Harvard University through the ITC Postdoctoral Fellowship. This work used computational resources provided by XSEDE allocation AST-190018, the Frontera allocation AST-20019, and additional resources provided by the University of Texas at Austin and the Texas Advanced Computing Center (TACC; DATA AVAILABILITY. The data supporting the plots within this article are available on reasonable request to the corresponding authors. A public version of the GIZMO code is available at
Group:Astronomy Department, TAPIR
Funding AgencyGrant Number
Harlan J. Smith McDonald ObservatoryUNSPECIFIED
Cottrell Scholar of Research Corporation27982
NASA Hubble FellowshipHST-HF2-51479
Harvard UniversityUNSPECIFIED
Texas Advanced Computing Center (TACC)UNSPECIFIED
Subject Keywords:stars: formation – stars: binaries: general – stars: statistics – MHD – turbulence
Record Number:CaltechAUTHORS:20220816-222001546
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116329
Deposited By: George Porter
Deposited On:18 Aug 2022 22:42
Last Modified:02 Jun 2023 01:28

Repository Staff Only: item control page