The role of magnetic fields in the formation of multiple massive stars

¹ Université Paris Cité, CNRS, AstroParticule et Cosmologie, 10 Rue Alice Domon et Léonie Duquet, 75013 Paris, France
e-mail: raphael.mignon-risse@apc.in2p3.fr
² Université Paris Cité, Université Paris-Saclay, CEA, CNRS, AIM, Orme des Merisiers, 91190 Gif-sur-Yvette, France
³ École Normale Supérieure de Lyon, CRAL, UMR CNRS 5574, Université Lyon I, 46 Allée d’Italie, 69364 Lyon Cedex 07, France

Received: 4 January 2023
Accepted: 7 March 2023

Abstract

Context. Most massive stars are located in multiple stellar systems. Magnetic fields are believed to be essential in the accretion and ejection processes around single massive protostars.

Aims. Our aim is to unveil the influence of magnetic fields in the formation of multiple massive stars, in particular on the fragmentation modes and properties of the multiple protostellar system.

Methods. Using RAMSES, we follow the collapse of a massive pre-stellar core with (non-ideal) radiation-(magneto-)hydrodynamics. We choose a setup that promotes multiple stellar system formation in order to investigate the influence of magnetic fields on the multiple system’s properties.

Results. In the purely hydrodynamical models, we always obtain (at least) binary systems following the fragmentation of an axisymmetric density bump in a Toomre-unstable disk around the primary sink. This result sets the frame for further study of stellar multiplicity. When more than two stars are present in these early phases, their gravitational interaction triggers mergers until there are only two stars left. The following gas accretion increases their orbital separation, and hierarchical fragmentation occurs so that both stars host a comparable disk as well as a stellar system that then also forms a similar disk. Disk-related fragmenting structures are qualitatively resolved when the finest resolution is approximately 1/20 of the disk radius. We identify several modes of fragmentation: Toomre-unstable disk fragmentation, arm-arm collision, and arm-filament collision. Disks grow in size until they fragment and become truncated as the newly formed companion gains mass. When including magnetic fields, the picture evolves: The primary disk is initially elongated into a bar; it produces less fragments; disk formation and arm-arm collision are captured at comparatively higher resolution; and arm-filament collision is absent. Magnetic fields reduce the initial orbital separation but do not affect its further evolution, which is mainly driven by gas accretion. With magnetic fields, the growth of individual disks is regulated even in the absence of fragmentation or truncation.

Conclusions. Hierarchical fragmentation is seen in unmagnetized and magnetized models. Magnetic fields, including non-ideal effects, are important because they remove certain fragmentation modes and limit the growth of disks, which is otherwise only limited through fragmentation.