There is no disk mass budget problem of planet formation

Abstract

The inferred dust masses from Class II protoplanetary disk observations are lower than or equal to the masses of the observed exoplanet systems. This poses the question of how planets form if their natal environments do not contain enough mass. This hypothesis has entered the literature as the "mass budget problem" of planet formation. We utilize numerical simulations of planet formation via pebble and gas accretion, including migration, in a viscously evolving protoplanetary disk, while tracing the time evolution of the dust mass. As expected, we find that the presence of a giant planet in the disk can influence the evolution of the disk itself and prevent rapid dust mass loss by trapping the dust outside its orbit. Early formation is crucial for giant planet formation, as we found in our previous work; therefore, our findings strengthen the hypothesis that planet formation has already occurred or is ongoing in Class II disks. Most importantly, we find that the optically thin dust mass significantly underestimates the total dust mass in the presence of a dust-trapping deep gap. We also show that the beam convolution would smear out the feature from a deep gap, especially if the planet forms in the inner disk. Such hidden dust mass, along with early planet formation, could be the answer to the hypothetical mass budget problem.

8 pages, 4 figures, submitted to A&A

References in corpus (33)

• A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation
• Separating gas-giant and ice-giant planets by halting pebble accretion
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• A stellar-mass-dependent drop in planet occurrence rates
• Planetesimal formation starts at the snow line
• A Circumplanetary Disk Around PDS70c
• 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
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• The Ophiuchus DIsc Survey Employing ALMA (ODISEA)-III: the evolution of substructures in massive discs at 3-5 au resolution
• The Mass Budget of Planet Forming Discs: Isolating the Epoch of Planetesimal Formation
• Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
• ALMA survey of Class II protoplanetary disks in Corona Australis: a young region with low disk masses
• Leaky dust traps: How fragmentation impacts dust filtering by planets
• New Constraints From Dust Lines On The Surface Densities Of Protoplanetary Disks
• Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• Mass constraints for 15 protoplanetary disks from HD 1-0
• Formation and evolution of a protoplanetary disk: combining observations, simulations and cosmochemical constraints
• How to make giant planets via pebble accretion
• Survey of Orion Disks with ALMA (SODA) I: Cloud-level demographics of 873 protoplanetary disks
• Photoevaporation of protoplanetary discs with PLUTO+PRIZMO I. Lower X-ray-driven mass-loss rates due to enhanced cooling
• Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario
• Composition of giant planets: the roles of pebbles and planetesimals
• Pebble accretion in class 0/I YSOs as a possible pathway for early planet formation
• Probing protoplanetary disk evolution in the Chamaeleon II region
• Which stars can form planets: Planetesimal formation at low metallicities
• A low accretion efficiency of planetesimals formed at planetary gap edges
• Millimeter emission in photoevaporating disks is determined by early substructures
• Do all gaps in protoplanetary discs host planets?
• Constraining giant planet formation with synthetic ALMA images of the Solar System's natal protoplanetary disk
• Distributions of gas and small and large grains in the LkH$\alpha 330$ disk trace a young planetary system

Cited by in corpus (4)

• Hidden under a warm blanket: If planets existed in protostellar disks, they would hardly produce observable substructures
• Numerical Insights into Disk Accretion, Eccentricity, and Kinematics in the Class 0 phase
• Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
• Spiral formation caused by late infall onto protoplanetary disks