Testing a New Model of Embedded Protostellar Disks Against Observation: The Majority of Orion Class 0/I Disks Are Likely Warm, Massive, and Gravitationally Unstable

Abstract

We formulate a parametrized model of embedded protostellar disks and test its ability to estimate disk properties by fitting dust-continuum observations. The main physical assumptions of our model are motivated by a recent theoretical study of protostellar disk formation; these assumptions include that the disk should be marginally gravitationally unstable, and that the dominant dust heating mechanism is internal accretion heating instead of external protostellar irradiation. These assumptions allow our model to reliably estimate the disk mass even when the observed emission is optically thick and to self-consistently determine disk (dust) temperature. Using our model to fit multi-wavelength observations of 156 disks in the VANDAM Orion survey, we find that the majority (57%) of this sample can be fit well by our model. Using our model, we produce new estimates of Orion protostellar disk properties. We find that these disks are generally warm and massive, with a typical star-to-disk mass ratio $M_{\mathrm{d}}/M_{\star }=\mathcal{O}(1)$ in Class 0/I. We also discuss why our estimates differ from those in previous studies and the implications of our results on disk evolution and fragmentation.

23 pages, 18 figures, 4 tables. Accepted for publication in ApJ

References in corpus (23)

• Gas- and dust evolution in protoplanetary disks
• The Burst Mode of Protostellar Accretion
• 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
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• A Millimeter Continuum Size-Luminosity Relationship for Protoplanetary Disks
• One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering
• Properties of gravitoturbulent accretion disks
• Decoupling of Magnetic Fields in Collapsing Protostellar Envelopes and Disk Formation and Fragmentation
• The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Disk Dust Mass Distributions across Protostellar Evolutionary Classes
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks
• Formation and Evolution of Disks around Young Stellar Objects
• Self-regulated gravitational accretion in protostellar discs
• Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud
• New Constraints From Dust Lines On The Surface Densities Of Protoplanetary Disks
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars V. A Characterization of Protostellar Multiplicity
• Formation and evolution of protostellar accretion discs. II. From 3D simulation to a simple semi-analytic model of Class 0/I discs
• The Rate, Amplitude and Duration of Outbursts from Class 0 Protostars in Orion
• Formation and evolution of protostellar accretion discs. I. Angular-momentum budget, gravitational self-regulation, and numerical convergence
• New Constraints on Protoplanetary Disk Gas Masses in Lupus
• Direct Formation of Planetary Embryos in Self-Gravitating Disks
• Hiding Signatures of Gravitational Instability in Protoplanetary Discs with Planets

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• Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247
• Chaotic Type I Migration in Turbulent Discs
• Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
• Dust hot spots at 10 au scales around the Class 0 binary IRAS 16293-2422 A: a departure from the passive irradiation model
• Revisiting collisional dust growth in Class 0/I protostellar disks: Sweep-up can convert a few $10M_{\oplus }$ of dust into kg pebbles in 0.1 Myr
• The compositions of the HR 8799 planets reflect accretion of both solids and metal-enriched gas
• Turbulent Transport of Dust Particles in Protostellar Disks: The Effect of Upstream Diffusion
• Formation of free-floating planetary mass objects via circumstellar disk encounters
• FAUST. XXVIII. High-Resolution ALMA Observations of Class 0/I Disks: Structure, Optical Depths, and Temperatures
• The Disk Population in a Distant Massive Protocluster