Early Initiation of Inner Solar System Formation at Dead-Zone Inner Edge
arXiv:2110.06739 · doi:10.3847/2041-8213/ac2f3b
Abstract
The inner solar system possesses a unique orbital structure in which there are no planets inside the Mercury orbit and the mass is concentrated around the Venus and Earth orbits. The origins of these features still remain unclear. We propose a novel concept that the building blocks of the inner solar system formed at the dead-zone inner edge in the early phase of the protosolar disk evolution, where the disk is effectively heated by the disk accretion. First, we compute the dust evolution in a gas disk with a dead zone and obtain the spatial distribution of rocky planetesimals. The disk is allowed to evolve both by a viscous diffusion and magnetically-driven winds. We find that the rocky planetesimals are formed in concentrations around 1 au with a total mass comparable to the mass of the current inner solar system in the early phase of the disk evolution within Myr. Based on the planetesimal distribution and the gas disk structure, we subsequently perform \textit{N}-body simulations of protoplanets to investigate the dynamical configuration of the planetary system. We find that the protoplanets can grow into planets without significant orbital migration because of the rapid clearing of the inner disk by the magnetically-driven disk winds. Our model can explain the origins of the orbital structure of the inner solar system. Several other features such as the rocky composition can also be explained by the early formation of rocky planetesimals.
arXiv comment8 pages, 6 figures, accepted for publication in ApJL
References in corpus (35)
- Streaming Instabilities in Protoplanetary Disks
- Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
- Building the Terrestrial Planets: Constrained Accretion in the Inner Solar System
- Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
- Formation of the Terrestrial Planets from a Narrow Annulus
- Planetesimal formation starts at the snow line
- Inside-Out Planet Formation
- Towards a Global Evolutionary Model of Protoplanetary Disks
- Evolution of Protoplanetary Discs with Magnetically Driven Disc Winds
- Fossilized condensation lines in the Solar System protoplanetary disk
- Close-in planetesimal formation by pile-up of drifting pebbles
- Bifurcation of planetary building blocks during Solar System formation
- Trapping Solids at the Inner Edge of the Dead Zone: 3-D Global MHD Simulations
- Four annular structures in a protostellar disk less than 500,000 years old
- On the water delivery to terrestrial embryos by ice pebble accretion
- Evolution of Snow Line in Optically Thick Protoplanetary Disks: Effects of Water Ice Opacity and Dust Grain Size
- From planetesimals to terrestrial planets: N-body simulations including the effects of nebular gas and giant planets
- Lunar and Terrestrial Planet Formation in the Grand Tack Scenario
- High-Temperature Ionization in Protoplanetary Disks
- Multiple Gaps in the Disk of the Class I Protostar GY 91
- 3D Radiation Non-ideal Magnetohydrodynamical Simulations Of The Inner Rim In Protoplanetary Disks
- Assembling the Building Blocks of Giant Planets around Intermediate Mass Stars
- Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds
- Temperature Structure in the Inner Regions of Protoplanetary Disks: Inefficient Accretion Heating Controlled by Nonideal Magnetohydrodynamics
- Dust-Pileup at the Dead-Zone Inner Edge and Implications for the Disk Shadow
- Dispersal of protoplanetary disks by the combination of magnetically driven and photoevaporative winds
- Formation of rocky and icy planetesimals inside and outside the snow line: Effects of diffusion, sublimation and back-reaction
- Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals
- MRI-active inner regions of protoplanetary discs. I. A detailed model of disc structure
- Substructure Formation in a Protostellar Disk of L1527 IRS
- Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system's terrestrial planets
- Inside-Out Planet Formation. IV. Pebble Evolution and Planet Formation Timescales
- Analytic Expressions for the Inner-Rim Structure of Passively Heated Protoplanetary Disks
- Close-in Super-Earths: The first and the last stages of planet formation in an MRI-accreting disc
- New growth mechanism of dust grains in protoplanetary disks with magnetically driven disk winds