There is no magnetic braking catastrophe: Low-mass star cluster and protostellar disc formation with non-ideal magnetohydrodynamics

Abstract

We present results from the first radiation non-ideal magnetohydrodynamics (MHD) simulations of low-mass star cluster formation that resolve the fragmentation process down to the opacity limit. We model 50~M${}_{\odot }$ turbulent clouds initially threaded by a uniform magnetic field with strengths of 3, 5 10 and 20 times the critical mass-to-magnetic flux ratio, and at each strength, we model both an ideal and non-ideal (including Ohmic resistivity, ambipolar diffusion and the Hall effect) MHD cloud. Turbulence and magnetic fields shape the large-scale structure of the cloud, and similar structures form regardless of whether ideal or non-ideal MHD is employed. At high densities ($10^6\lesssim n_{\mathrm{H}}\lesssim 10^{11}$~cm${}^{-3}$), all models have a similar magnetic field strength versus density relation, suggesting that the field strength in dense cores is independent of the large-scale environment. Albeit with limited statistics, we find no evidence for the dependence of the initial mass function on the initial magnetic field strength, however, the star formation rate decreases for models with increasing initial field strengths; the exception is the strongest field case where collapse occurs primarily along field lines. Protostellar discs with radii $\gtrsim 20$~au form in all models, suggesting that disc formation is dependent on the gas turbulence rather than on magnetic field strength. We find no evidence for the magnetic braking catastrophe, and find that magnetic fields do not hinder the formation of protostellar discs.

arXiv comment24 pages, 19 figures. Accepted for publication in MNRAS. Videos available at https://www.youtube.com/watch?v=CLhmaOhj5RU&list=PLwI7am9c6sBjW69kfhfRDMR3Gz6nzOPOi

References in corpus (113)

• The chemical composition of the Sun
• Theory of Star Formation
• Low Temperature Opacities
• The Stellar IMF from Turbulent Fragmentation
• Cold Dark Clouds: The Initial Conditions for Star Formation
• Modelling Accretion in Protobinary Systems
• Density, Velocity, and Magnetic Field Structure in Turbulent Molecular Cloud Models
• The Formation of a Star Cluster: Predicting the Properties of Stars and Brown Dwarfs
• The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations
• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Smoothed Particle Hydrodynamics and Magnetohydrodynamics
• Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation
• Large-Scale Structure of the Molecular Gas in Taurus Revealed by High Linear Dynamic Range Spectral Line Mapping
• Stellar, Brown Dwarf, and Multiple Star Properties from Hydrodynamical Simulations of Star Cluster Formation
• Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
• Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
• An energy-conserving formalism for adaptive gravitational force softening in SPH and N-body codes
• On the diversity and statistical properties of protostellar discs
• The Effects of Radiative Transfer on Low-Mass Star Formation
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• Protostellar disk formation and transport of angular momentum during magnetized core collapse
• Collapse of Magnetized Singular Isothermal Toroids: II. Rotation and Magnetic Braking
• The Importance of Radiative Feedback for the Stellar Initial Mass Function
• Magnetic Braking and Protostellar Disk Formation: The Ideal MHD Limit
• Before the first supernova: combined effects of HII regions and winds on molecular clouds
• The impact of magnetic fields on single and binary star formation
• The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows
• Dispersal of molecular clouds by ionising radiation
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• Collapse of massive magnetized dense cores using radiation-magneto-hydrodynamics: early fragmentation inhibition
• Stellar Feedback in Molecular Clouds and its Influence on the Mass Function of Young Star Clusters
• Radiation-Hydrodynamic Simulations of the Formation of Orion-Like Star Clusters II. The Initial Mass Function from Winds, Turbulence, and Radiation
• Collapse, outflows and fragmentation of massive, turbulent and magnetized prestellar barotropic cores
• The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer
• Collapse and Fragmentation in Finite Sheets
• The Fragmentation of Magnetized, Massive Star-Forming Cores with Radiative Feedback
• Magnetic processes in a collapsing dense core. II Fragmentation. Is there a fragmentation crisis ?
• A Simple Law of Star Formation
• Smoothed Particle Magnetohydrodynamics II. Variational principles and variable smoothing length terms
• The effect of magnetic fields on star cluster formation
• The Magnetic Field in Taurus Probed by Infrared Polarization
• Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe?
• Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation
• Gravitational collapse of magnetized clouds. I. Ideal MHD accretion flow
• Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
• Magnetic fields during the early stages of massive star formation - I. Accretion and disk evolution
• Effects of Ohmic and ambipolar diffusion on the formation and evolution of the first cores, protostars and circumstellar discs
• Smoothed Particle Magnetohydrodynamics III. Multidimensional tests and the div B = 0 constraint
• Numerical requirements for simulations of self gravitating and non-self gravitating disks
• Spatially Resolved Magnetic Field Structure in the Disk of a T Tauri Star
• Inefficient star formation: The combined effects of magnetic fields and radiative feedback
• ALMA Reveals Transition of Polarization Pattern with Wavelength in HL Tau's Disk
• The influence of turbulence during magnetized core collapse and its consequences on low-mass star formation
• Bimodality of circumstellar disk evolution induced by Hall current
• Turbulence-induced disc formation in strongly magnetised cloud cores
• The Origin and Formation of the Circumstellar Disk
• Star Cluster Formation in Turbulent, Magnetized Dense Clumps with Radiative and Outflow Feedback
• Smoothed Particle Magnetohydrodynamics I. Algorithms and tests in one dimension
• The Internal Energy for Molecular Hydrogen in Gravitationally Unstable Protoplanetary Disks
• A faster algorithm for smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
• Disc formation in turbulent massive cores: Circumventing the magnetic braking catastrophe
• The statistical properties of stars and their dependence on metallicity
• Optical polarimetry toward the Pipe nebula: Revealing the importance of the magnetic field
• The statistical properties of stars and their dependence on metallicity: the effects of opacity
• Magnetic Fields in Diffuse H I and Molecular Clouds
• Protostellar birth with ambipolar and ohmic diffusion
• Numerical Simulations of Turbulent Molecular Clouds Regulated by Reprocessed Radiation Feedback from Nascent Super Star Clusters
• The dependence of star formation on initial conditions and molecular cloud structure
• A Sub-arcsecond Survey Toward Class 0 Protostars in Perseus: Searching for Signatures of Protostellar Disks
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• Moving mesh simulations of star forming cores in magneto-gravo-turbulence
• Detailed Interstellar Polarimetric Properties of the Pipe Nebula at Core Scales
• ALMA's Polarized View of 10 Protostars in the Perseus Molecular Cloud
• The role of magnetic fields in the formation of protostellar discs
• On the Origin of Stellar Masses
• Photoionisation Feedback in a Self-Gravitating, Magnetised, Turbulent Cloud
• Exposed Long-lifetime First-core: A New Model of First Cores Based on Radiation Hydrodynamics
• Disruption of Molecular Clouds by Expansion of Dusty H II Regions
• The Effects of Magnetic Fields and Protostellar Feedback on Low-mass Cluster Formation
• Nonlinear Evolution of Global Hydrodynamic Shallow-Water Instability in Solar Tachocline
• Detection of a Bipolar Molecular Outflow Driven by a Candidate First Hydrostatic Core
• The impact of the Hall effect during cloud core collapse:implications for circumstellar disk evolution
• Planck intermediate results. XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• Stellar mass spectrum within massive collapsing clumps II. Thermodynamics and tidal forces of the first Larson core
• Constrained hyperbolic divergence cleaning in smoothed particle magnetohydrodynamics with variable cleaning speeds
• ALMA observations of the kinematics and chemistry of disc formation
• On the Indeterministic Nature of Star Formation on the Cloud Scale
• Stellar mass spectrum within massive collapsing clumps I. Influence of the initial conditions
• Smoothed Particle Magnetohydrodynamics IV - Using the Vector Potential
• Protostars, multiplicity, and disk evolution in the Corona Australis region: A Herschel Gould Belt Study
• Disc formation in turbulent cloud cores: is magnetic flux loss necessary to stop the magnetic braking catastrophe or not?
• The JCMT Gould Belt Survey: SCUBA-2 observations of radiative feedback in NGC1333
• The observable prestellar phase of the IMF
• Ambipolar diffusion in smoothed particle magnetohydrodynamics
• A switch to reduce resistivity in smoothed particle magnetohydrodynamics
• NICIL: A stand alone library to self-consistently calculate non-ideal magnetohydrodynamic coefficients in molecular cloud cores
• Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics
• The impact of non-ideal magnetohydrodynamics on binary star formation
• The effect of the virial state of molecular clouds on the influence of feedback from massive stars
• Combining radiative transfer and diffuse interstellar medium physics to model star formation
• Evolution of Blister-Type HII Regions in a Magnetized Medium
• 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
• On the origin of magnetic fields in stars
• Evidence for disks at an early stage in class 0 protostars?
• The dependence of protostar formation on the geometry and strength of the initial magnetic field
• Stellar mass spectrum within massive collapsing clumps III. Effects of temperature and magnetic field
• Does turbulence determine the initial mass function?
• Shaken and stirred: the effects of turbulence and rotation on disc and outflow formation during the collapse of magnetised molecular cloud cores
• Sink particle radiative feedback in smoothed particle hydrodynamics models of star formation
• The dependence of stellar properties on initial cloud density
• Investigating prescriptions for artificial resistivity in smoothed particle magnetohydrodynamics

Cited by in corpus (51)

• STARFORGE: Toward a comprehensive numerical model of star cluster formation and feedback
• A protostellar system fed by a streamer of 10,500 au length
• PRODIGE -- Envelope to disk with NOEMA I. A 3000 au streamer feeding a Class I protostar
• The importance of magnetic fields for the initial mass function of the first stars
• STARFORGE: The effects of protostellar outflows on the IMF
• What determines the formation and characteristics of protoplanetary discs?
• Effects of the environment and feedback physics on the initial mass function of stars in the STARFORGE simulations
• The Role of Outflows, Radiation Pressure, and Magnetic Fields in Massive Star Formation
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Magnetic field amplification in accretion discs around the first stars: implications for the primordial IMF
• Formation and evolution of protostellar accretion discs. I. Angular-momentum budget, gravitational self-regulation, and numerical convergence
• Non-ideal magnetohydrodynamics vs turbulence I: Which is the dominant process in protostellar disc formation?
• Can magnetized turbulence set the mass scale of stars?
• The JCMT BISTRO survey: alignment between outflows and magnetic fields in dense cores/clumps
• Ionization: a possible explanation for the difference of mean disk sizes in star-forming regions
• Survey of Gravitationally lensed Objects in HSC Imaging (SuGOHI) -- VII. Discovery and Confirmation of Three Strongly Lensed Quasars
• The contribution of binary star formation via core-fragmentation on protostellar multiplicity
• Disc population synthesis: Decrease in the solid mass reservoir through pebble drift
• Binary-induced spiral arms inside the disc cavity of AB Aurigae
• Non-ideal magnetohydrodynamics vs turbulence II: Which is the dominant process in stellar core formation?
• Do we need non-ideal magnetohydrodynamics to model protostellar discs?
• Angular Momenta, Magnetization, and Accretion of Protostellar Cores
• On the origin of magnetic fields in stars II: The effect of numerical resolution
• Spirals, shadows & precession in HD 100453 -- II. The hidden companion
• The statistical properties of stars at redshift, z=5, compared with the present epoch
• The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds
• Transition from ordered pinched to warped magnetic field on a 100 au scale in the Class 0 protostar B335
• Rogue planets and brown dwarfs: Predicting the populations of free-floating planetary mass objects observable with JWST
• Variation of the low-mass end of the stellar initial mass function with redshift and metallicity
• The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency
• Growth of Magnetorotational Instability in Circumstellar Disks around Class 0 Protostars
• The statistical properties of protostellar discs and their dependence on metallicity
• Dust Motion and Possibility of Dust Growth in a Growing Circumstellar Disk
• Do simulated molecular clouds look like real ones?
• Are magnetic fields universal in O-type multiple systems?
• No impact of core-scale magnetic field, turbulence, or velocity gradient on sizes of protostellar disks in Orion A
• Observational Signatures of Circumbinary Discs I: Kinematics
• Orbital parameters and activity of ZZ Tau -- a low mass young binary with circumbinary disc
• Time evolution of the galactic $B-\rho$ relation: the impact of the magnetic field morphology
• Protostellar disk accretion in turbulent filaments
• Turbulence and its connection to episodic accretion in binary YSOs
• Gas and star kinematics in cloud-cloud collisions
• The High-resolution Accretion Disks of Embedded protoStars (HADES) simulations. I. Impact of Protostellar Magnetic Fields on the Accretion Modes
• Star-forming environments in smoothed particle magnetohydrodynamics simulations I: Clump extraction and properties
• Late encounter-events as a source of disks and spiral structures -- Forming second generation disks
• Sulfur oxides tracing streamers and shocks at low mass protostellar disk-envelope interfaces
• The factors that influence protostellar multiplicity I: Gas temperature, density, and mass in Perseus with Nobeyama
• Non-ideal MHD and protostellar feedback effects on disc formation and evolution in numerical simulations of star cluster formation
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars VI. Insights from Radiative Transfer Modeling
• Effects of magnetic field orientations in dense cores on gas kinematics in protostellar envelopes
• Magnetic reconnection in partially ionized plasmas