Presentation #411.05 in the session “Origins, Formation and Dynamical Systems”. Cross-listed as presentation #506.03.
Dust envelopes surrounding chondrules encode important data on the formation of planetesimals. It is widely accepted that these envelopes accreted onto chondrule surfaces while free-floating in the solar nebula. One of the dynamical processes under current scrutiny is the compaction that primordial chondrule dust envelopes experienced after accretion. While theoretical and experimental studies show that envelope accretion produces relatively porous structures, the dust envelopes observed in chondrite samples are generally compact. The compaction mechanism is not yet fully determined. The purpose of this work is to specify the degree of envelope compaction and overall morphology resulting from one specific process: high-speed collisions between a rimmed chondrule and a dust cloud.
We perform 2D numerical simulations with the iSALE2D shock physics code. A portion of a chondrule is modeled as a dunite slab, with an initial porous layer of dust on the slab surface. The dust particles are modeled as dunite disks with diameters between 2.4 and 3.6 μm. The combined chondrule/dust structure undergoes a collision with a dust cloud containing the same type of grains as the chondrule dust layer. In order to probe a variety of collision scenarios, we change the particle fraction, fp, in the dust cloud (0.01 – 0.30), the collision speed (750 m/s – 3000 m/s), and the cohesion of the intact material (5 x 105 Pa – 108 Pa). Preliminary results show that the original dust layer on the chondrule surface undergoes significant compaction for all the examined collision speeds. However, the morphology of the resulting layer differs considerably for different dust cloud particle fractions. In the case of small fp, filamentary dust structures are formed as a result of the collision, and remain through the duration of the simulation. In contrast, no filaments are observed for large fp. Overall, the topography of the compacted dust layer is more complex for small fp than for large fp. In all cases, appreciable deformation of the chondrule surface occurs, with indentations of varying depths that resemble those observed in the Paris CM chondrite. Upon impact, temperatures in the dust layer rise markedly above the initial temperature of 300 K, at which the chondrule remains throughout the simulation. The dust temperature can reach ~700 K in a 3000-m/s collision with fp = 0.01 (see figures).
Further work remains to compute the porosity of the compacted dust layer. The porosity will be compared to values measured in chondrite samples and in upcoming high-speed-collision experiments that use chondrule analogs.