Forbidden planetesimals
arXiv:2305.03562 · doi:10.1051/0004-6361/202245499
Abstract
Planetesimals are born fragile and are subject to destruction by wind erosion as they move through the gas of a protoplanetary disk. In microgravity experiments, we determined the shear stress necessary for erosion of a surface consisting of 1 mm dust pebbles down to 1 Pa ambient pressure. This is directly applicable to protoplanetary disks. Even pebble pile planetesimals with low eccentricities of 0.1 cannot survive inside of 1 au in a minimum-mass solar nebula, and safe zones for planetesimals with higher eccentricities are located even farther out.
References in corpus (27)
- Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70
- The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
- Forming Planetesimals in Solar and Extrasolar Nebulae
- Planetesimal formation by sweep-up: How the bouncing barrier can be beneficial to growth
- Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles
- Formation of planetary systems by pebble accretion and migration: Growth of gas giants
- Gravoturbulent Planetesimal Formation: The Positive Effect of long-lived Zonal Flows
- Sticking Properties of Silicates in Planetesimal Formation Revisited
- Experimental Study on Bouncing Barriers in Protoplanetary Disks
- Pebbles versus planetesimals: the outcomes of population synthesis models
- Understanding planet formation using microgravity experiments
- Saltation under Martian Gravity and its Influence on the Global Dust Distribution
- The Streaming Instability Cannot Form Planetesimals from mm-size Grains in Pressure Bumps
- Failed Growth at the Bouncing Barrier in Planetesimal Formation
- Seeding the Formation of Mercurys: An Iron-sensitive Bouncing Barrier in Disk Magnetic Fields
- The role of pebble fragmentation in planetesimal formation II. Numerical simulations
- Is There a Temperature Limit in Planet Formation at 1000 K?
- The aeolian-erosion barrier for the growth of metre-size objects in protoplanetary-discs
- Wind erosion on Mars and other small terrestrial planets
- Growing into and out of the bouncing barrier in planetesimal formation
- A Smoking Gun for Planetesimal Formation: Charge Driven Growth into a New Size Range
- Are Pebble Pile Planetesimals Doomed?
- Planetesimals in Rarefied Gas: Wind Erosion in Slip Flow
- Observation of bottom-up formation for charged grain aggregates related to pre-planetary evolution beyond the bouncing barrier
- Erosion of planetesimals by gas flow
- Destruction of eccentric planetesimals by ram pressure and erosion
- Accretion of eroding pebbles and planetesimals in planetary envelopes