Forming chondrules in impact splashes. I. Radiative cooling model

Abstract

The formation of chondrules is one of the oldest unsolved mysteries in meteoritics and planet formation. Recently an old idea has been revived: the idea that chondrules form as a result of collisions between planetesimals in which the ejected molten material forms small droplets which solidify to become chondrules. Pre-melting of the planetesimals by radioactive decay of 26Al would help producing sprays of melt even at relatively low impact velocity. In this paper we study the radiative cooling of a ballistically expanding spherical cloud of chondrule droplets ejected from the impact site. We present results from a numerical radiative transfer models as well as analytic approximate solutions. We find that the temperature after the start of the expansion of the cloud remains constant for a time t_cool and then drops with time t approximately as T ~ T_0[(3/5)t/t_cool+ 2/5]^(-5/3) for t>t_cool. The time at which this temperature drop starts t_cool depends via an analytical formula on the mass of the cloud, the expansion velocity and the size of the chondrule. During the early isothermal expansion phase the density is still so high that we expect the vapor of volatile elements to saturate so that no large volatile losses are expected.

References in corpus (7)

• A low mass for Mars from Jupiter's early gas-driven migration
• Chondrule Formation in Bow Shocks around Eccentric Planetary Embryos
• Thermal Histories of Chondrules in Solar Nebula Shocks
• On the aerodynamic redistribution of chondrite components in protoplanetary disks
• Short Circuits in Thermally Ionized Plasmas: A Mechanism for Intermittent Heating of Protoplanetary Disks
• High-Temperature Processing of Solids Through Solar Nebular Bow Shocks: 3D Radiation Hydrodynamics Simulations with Particles
• A critical analysis of shock models for chondrule formation

Cited by in corpus (19)

• The Impact of Dust Evolution and Photoevaporation on Disk Dispersal
• The effects of short-lived radionuclides and porosity on the early thermo-mechanical evolution of planetesimals
• Impact splash chondrule formation during planetesimal recycling
• Formation and Evolution of Disks around Young Stellar Objects
• Leaky dust traps: How fragmentation impacts dust filtering by planets
• Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
• Thermal History Of Cbb Chondrules And Cooling Rate Distributions Of Ejecta Plumes
• Harvesting the decay energy of ${}^{26}$Al to drive lightning discharge in protoplanetary discs
• Compound chondrule formation in optically thin shock waves
• Forming chondrules in impact splashes - II Volatile retention
• Can chondrules be produced by the interaction of Jupiter with the protosolar disk?
• Ejection of Chondrules from Fluffy Matrices
• Chondrules from high-velocity collisions: thermal histories and the agglomeration problem
• The motion of chondrules and other particles in a protoplanetary disc with temperature fluctuations
• Chondrule Formation by the Jovian Sweeping Secular Resonance
• Dust concentration and chondrule formation
• The Properties of Planetesimal Collisions under Jupiter's Perturbation and the Application to Chondrule Formation via Impact Jetting
• Chondrule formation by collisions of planetesimals containing volatiles triggered by Jupiter's formation
• Chondrites as thermal and mechanical archives of accretion processes in the Solar protoplanetary disk