The role of initial magnetic field structure in the launching of protostellar jets

Abstract

Magnetic fields are known to play a crucial role in the star formation process, particularly in the formation of jets and outflows from protostellar discs. The magnetic field structure in star forming regions is not always uniform and ordered, often containing regions of magnetic turbulence. We present grid-based, magneto-hydrodynamical simulations of the collapse of a 1${\mathrm{M}}_{\odot }$ cloud core, to investigate the influence of complex magnetic field structures on outflow formation, morphology and efficiency. We compare three cases: a uniform field, a partially turbulent field and a fully turbulent field, with the same magnetic energy in all three cases. We find that collimated jets are produced in the uniform-field case, driven by a magneto-centrifugal mechanism. Outflows also form in the partially turbulent case, although weaker and less collimated, with an asymmetric morphology. The outflows launched from the partially turbulent case carry the same amount of mass as the uniform-field case but at lower speeds, having only have 71$\%$ of the momentum of the uniform-field case. In the case of a fully turbulent field, we find no significant outflows at all. Moreover, the turbulent magnetic field initially reduces the accretion rate and later induces fragmentation of the disc, forming multiple protostars. We conclude that a uniform poloidal component of the magnetic field is necessary for the driving of jets.

arXiv comment12 pages, 6 figures, accepted for publication in MNRAS

References in corpus (84)

• Theory of Star Formation
• Control of star formation by supersonic turbulence
• Astrophysical magnetic fields and nonlinear dynamo theory
• Stellar Multiplicity
• A Multi-Code Analysis Toolkit for Astrophysical Simulation Data
• Interstellar Turbulence I: Observations and Processes
• Comparing the statistics of interstellar turbulence in simulations and observations: Solenoidal versus compressive turbulence forcing
• The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations
• An Unsplit Godunov Method for Ideal MHD via Constrained Transport
• Thermal and Fragmentation Properties of Star-forming Clouds in Low-metallicity Environments
• The Universality of Turbulence in Galactic Molecular Clouds
• Radiative torques: Analytical Model and Basic Properties
• Modeling Collapse and Accretion in Turbulent Gas Clouds: Implementation and Comparison of Sink Particles in AMR and SPH
• Turbulent molecular clouds
• The Big Problems in Star Formation: the Star Formation Rate, Stellar Clustering, and the Initial Mass Function
• The Effects of Radiative Transfer on Low-Mass Star Formation
• Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• Protostellar disk formation and transport of angular momentum during magnetized core collapse
• A study of high velocity molecular outflows with an up-to-date sample
• A new Jeans resolution criterion for (M)HD simulations of self-gravitating gas: Application to magnetic field amplification by gravity-driven turbulence
• Simulating the formation of molecular clouds. II. Rapid formation from turbulent initial conditions
• Inefficient star formation through turbulence, magnetic fields and feedback
• The impact of magnetic fields on single and binary star formation
• Mach Number Dependence of Turbulent Magnetic Field Amplification: Solenoidal versus Compressive Flows
• Outflows and Jets from Collapsing Magnetized Cloud Cores
• Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites
• On Why Disks Generate Magnetic Towers and Collimate Jets
• The conductivity of dense molecular gas
• The spine of the swan: A Herschel study of the DR21 ridge and filaments in Cygnus X
• Disk formation during collapse of magnetized protostellar cores
• The generation of strong magnetic fields during the formation of the first stars
• Modeling jet and outflow feedback during star cluster formation
• A robust numerical scheme for highly compressible magnetohydrodynamics: Nonlinear stability, implementation and tests
• Modelling CO formation in the turbulent interstellar medium
• Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe?
• Magnetic field amplification in turbulent astrophysical plasmas
• Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
• The JCMT BISTRO Survey: The magnetic field strength in the Orion A filament
• Irradiated Herbig-Haro Jets in the Orion Nebula and Near NGC 1333
• Does Magnetic Field-Rotation Misalignment Solve the Magnetic Braking Catastrophe in Protostellar Disk Formation?
• The Small-Scale Dynamo and Non-Ideal MHD in Primordial Star Formation
• Inefficient star formation: The combined effects of magnetic fields and radiative feedback
• The influence of turbulence during magnetized core collapse and its consequences on low-mass star formation
• Star formation in metal-poor gas clouds
• Bimodality of circumstellar disk evolution induced by Hall current
• Planck intermediate results. XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps
• TURBULENCE IN MOLECULAR CLOUDS
• Protostellar birth with ambipolar and ohmic diffusion
• Alignment Between Flattened Protostellar Infall Envelopes and Ambient Magnetic Fields
• ALMA observations of dust polarization and molecular line emission from the Class 0 protostellar source Serpens SMM1
• DR 21(OH): a highly fragmented, magnetized, turbulent dense core
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• The Turbulence Spectrum of Molecular Clouds in the Galactic Ring Survey: A Density-Dependent PCA Calibration
• Gravitational collapse of magnetized clouds II. The role of Ohmic dissipation
• ALMA's Polarized View of 10 Protostars in the Perseus Molecular Cloud
• Tree-based solvers for adaptive mesh refinement code FLASH - I: gravity and optical depths
• Protostellar Outflows and Radiative Feedback from Massive Stars. II. Feedback, Star Formation Efficiency, and Outflow Broadening
• Collimated jets from the first core
• Outflows and mass accretion in collapsing dense cores with misaligned rotation axis and magnetic field
• Protostellar Disk Formation Enabled by Weak, Misaligned Magnetic Fields
• The Star Formation Rate of Molecular Clouds
• The First Jet in the Universe: Protostellar Jets from the First Stars
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• The Hall effect in star formation
• Constrained hyperbolic divergence cleaning in smoothed particle magnetohydrodynamics with variable cleaning speeds
• On the Role of Pseudodisk Warping and Reconnection in Protostellar Disk Formation in Turbulent Magnetized Cores
• Effect of Angular Momentum Alignment and Strong Magnetic Fields on the Formation of Protostellar Disks
• The Small-Scale Dynamo at Low Magnetic Prandtl Numbers
• Magnetic fields in the massive dense cores of DR21 filament: weakly magnetized cores in a strongly magnetized filament
• The small-scale dynamo: Breaking universality at high Mach numbers
• Entrainment Mechanisms for Outflows in the L1551 Star-Forming Region
• The Link between Magnetic Fields and Cloud/Star Formation
• Isothermal Fragmentation: Is there a low-mass cut-off?
• Modeling Dust Polarization Observations of Molecular Clouds through MHD Simulations
• Smoothed particle magnetohydrodynamic simulations of protostellar outflows with misaligned magnetic field and rotation axes
• Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores
• The effect of extreme ionisation rates during the initial collapse of a molecular cloud core
• Binary Star Formation and the Outflows from their Discs
• The dependence of protostar formation on the geometry and strength of the initial magnetic field
• Hydrodynamical simulations of the decay of high-speed molecular turbulence. II. Divergence from isothermality
• Shaken and stirred: the effects of turbulence and rotation on disc and outflow formation during the collapse of magnetised molecular cloud cores
• Centrifugally driven winds from protostellar accretion discs. I - Formulation and initial results
• The Effects of Large-Scale Magnetic Fields on Disk Formation and Evolution

Cited by in corpus (20)

• STARFORGE: Toward a comprehensive numerical model of star cluster formation and feedback
• The importance of magnetic fields for the initial mass function of the first stars
• Magnetic Fields in the Formation of the First Stars. I. Theory vs. Simulation
• Magnetic field amplification in accretion discs around the first stars: implications for the primordial IMF
• Magnetic field fluctuations in anisotropic, supersonic turbulence
• Non-ideal magnetohydrodynamics vs turbulence I: Which is the dominant process in protostellar disc formation?
• Filaments and striations: anisotropies in observed, supersonic, highly-magnetised turbulent clouds
• Molecular cloud formation by compression of magnetized turbulent gas subjected to radiative cooling
• Magnetohydrodynamic effect on first star formation: prestellar core collapse and protostar formation
• A new method for measuring the 3D turbulent velocity dispersion of molecular clouds
• The role of magnetic fields in the formation of multiple massive stars
• Non-ideal MHD simulations of subcritical prestellar cores with non-equilibrium chemistry
• The dependence of episodic accretion on eccentricity during the formation of binary stars
• Non-ideal magnetohydrodynamic simulations of the first star formation: the effect of ambipolar diffusion
• PDM relativistic quantum oscillator in Einstein-Maxwell-Lambda space-time
• Physical conditions for dust grain alignment in Class 0 protostellar cores II. The role of the radiation field in models aligning/disrupting dust grains
• Protostellar spin-up and fast rotator formation through binary star formation
• Star-forming environments in smoothed particle magnetohydrodynamics simulations I: Clump extraction and properties
• Wide-binary eccentricity distribution in young star clusters: dependence on the binary separation and mass
• Protostellar disc structure and dynamics during star formation from cloud-scale initial conditions