Protoplanetary disk birth in massive star forming clumps: the essential role of the magnetic field

Abstract

Protoplanetary disks form through angular momentum conservation in collapsing dense cores. In this work, we perform the first simulations with a maximal resolution down to the astronomical unit (au) of protoplanetary disk formation, through the collapse of 1000 solar mass clumps, treating self-consistently both non-ideal magnetohydrodynamics with ambipolar diffusion as well as radiative transfer in the flux-limited diffusion approximation including stellar feedback. Using the adaptive mesh-refinement code RAMSES, we investigate the influence of the magnetic field on the disks properties with three models. We show that, without magnetic fields, a population dominated by large disks is formed, which is not consistent with Class 0 disk properties as estimated from observations. The inclusion of magnetic field leads, through magnetic braking, to a very different evolution. When it is included, small < 50 au disks represent about half the population. In addition, about ~ 70% of the stars have no disk in this case which suggests that our resolution is still insufficient to preserve the smaller disks. With ambipolar diffusion, the proportion of small disks is also prominent and we report a flat mass distribution around 0.01-0.1 solar mass and a typical disk-to-star mass ratios of ~0.01-0.1. This work shows that the magnetic field and its evolution plays a prominent role in setting the initial properties of disk populations.

13 pages, 5 figures, accepted for publication in The Astrophysical Journal Letters

References in corpus (14)

• Protoplanetary Disk Structures in Ophiuchus
• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• On the diversity and statistical properties of protostellar discs
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• ATLASGAL --- towards a complete sample of massive star forming clumps
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ }<\ell <67.0^{\circ }$)
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Non-Ideal Magnetohydrodynamic Effects and Early Formation of Circumstellar Disks
• Magnetic processes in a collapsing dense core. II Fragmentation. Is there a fragmentation crisis ?
• Towards a more realistic sink particle algorithm for the RAMSES code
• Magnetically self-regulated formation of early protoplanetary discs
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Effect of Angular Momentum Alignment and Strong Magnetic Fields on the Formation of Protostellar Disks
• Non-ideal magnetohydrodynamics vs turbulence I: Which is the dominant process in protostellar disc formation?

Cited by in corpus (30)

• PRODIGE -- Envelope to disk with NOEMA I. A 3000 au streamer feeding a Class I protostar
• Protostellar collapse simulations in spherical geometry with dust coagulation and fragmentation
• The evolution of protoplanetary discs in star formation and feedback simulations
• Magnetically regulated collapse in the B335 protostar? II. Observational constraints on gas ionization and magnetic field coupling
• Probing the physics of star formation (ProPStar): I. First resolved maps of the electron fraction and cosmic-ray ionization rate in NGC 1333
• Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level
• How magnetic field and stellar radiative feedback influences the collapse and the stellar mass spectrum of a massive star forming clump
• The birth and early evolution of a low mass protostar
• Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau's Complex Kilo-au Environment
• Fragmentation with Discontinuous Galerkin schemes: Non-linear fragmentation
• The role of magnetic fields in the formation of multiple massive stars
• Probing the eccentricity in protostellar discs -- Modeling kinematics and morphologies
• The time evolution of $M_{\mathrm{d}}/\dot{M}$ in protoplanetary discs as a way to disentangle between viscosity and MHD winds
• Accuracy of ALMA estimates of young disk radii and masses. Predicted observations from numerical simulations
• FAUST XX. The chemical structure and temperature profile of the IRAS 4A2 hot corino at 20-50 au
• A giant planet shaping the disk around the very low-mass star CIDA 1
• Filling in the Gaps: Can Gravitationally Unstable Discs Form the Seeds of Gas Giant Planets?
• Formation of low mass protostars and their circumstellar disks
• Disk fragmentation around a massive protostar: a comparison of two three-dimensional codes
• Dust evolution during the protostellar collapse: influence on the coupling between the neutral gas and the magnetic field
• Birth of magnetized low-mass protostars and circumstellar disks
• Protostellar disk accretion in turbulent filaments
• FAUST. XXVIII. High-Resolution ALMA Observations of Class 0/I Disks: Structure, Optical Depths, and Temperatures
• The evolution of the $M_{\mathrm{d}}-M_{\star }$ and $\dot{M}-M_{\star }$ correlations traces protoplanetary disc dispersal
• Fragmentation of Dense Rotation-Dominated Structures Fed by Collapsing Gravomagneto-Sheetlets and Origin of Misaligned 100 au-Scale Binaries and Multiple Systems
• Density profile of a self-gravitating polytropic turbulent fluid in a rotating disk near to the cloud core
• Protostellar disc structure and dynamics during star formation from cloud-scale initial conditions
• Warps survive beyond fly-by encounters in protoplanetary disks. RW Aur A as a case study
• Star Forming Regions
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars VI. Insights from Radiative Transfer Modeling