Gravity-dominated Collisions: A Model for the Largest Remnant Masses with Treatment for “Hit and Run” and Density Stratification
dc.contributor.author | Gabriel, Travis S. J. | |
dc.contributor.author | Jackson, Alan P. | |
dc.contributor.author | Asphaug, Erik | |
dc.contributor.author | Reufer, Andreas | |
dc.contributor.author | Jutzi, Martin | |
dc.contributor.author | Benz, Willy | |
dc.date.accessioned | 2020-07-20T21:49:19Z | |
dc.date.available | 2020-07-20T21:49:19Z | |
dc.date.issued | 2020-03-24 | |
dc.identifier.citation | Travis S. J. Gabriel et al 2020 ApJ 892 40 | en_US |
dc.identifier.issn | 0004-637X | |
dc.identifier.doi | 10.3847/1538-4357/ab528d | |
dc.identifier.uri | http://hdl.handle.net/10150/641911 | |
dc.description.abstract | We develop empirical relationships for the accretion and erosion of colliding gravity-dominated bodies of various compositions under conditions expected in late-stage solar system formation. These are fast, easily coded relationships based on a large database of smoothed particle hydrodynamics (SPH) simulations of collisions between bodies of different compositions, including those that are water rich. The accuracy of these relations is also comparable to the deviations of results between different SPH codes and initial thermal/rotational conditions. We illustrate the paucity of disruptive collisions between major bodies, as compared to collisions between less massive planetesimals in late-stage planet formation, and thus focus on more probable, low-velocity collisions, though our relations remain relevant to disruptive collisions as well. We also pay particular attention to the transition zone between merging collisions and those where the impactor does not merge with the target, but continues downrange, a "hit-and-run" collision. We find that hit-and-run collisions likely occur more often in density-stratified bodies and across a wider range of impact angles than suggested by the most commonly used analytic approximation. We also identify a possible transitional zone in gravity-dominated collisions where larger bodies may undergo more disruptive collisions when the impact velocity exceeds the sound speed, though understanding this transition warrants further study. Our results are contrary to the commonly assumed invariance of total mass (scale), density structure, and material composition on the largest remnants of giant impacts. We provide an algorithm for adopting our model into N-body planet formation simulations, so that the mass of growing planets and debris can be tracked. | en_US |
dc.language.iso | en | en_US |
dc.publisher | IOP PUBLISHING LTD | en_US |
dc.rights | Copyright © 2020. The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. | en_US |
dc.rights.uri | https://creativecommons.org/licenses/by/3.0/ | |
dc.subject | Impact phenomena | en_US |
dc.subject | Planetary science | en_US |
dc.subject | Planet formation | en_US |
dc.subject | Hydrodynamics | en_US |
dc.subject | Hydrodynamical simulations | en_US |
dc.subject | Inner planets | en_US |
dc.title | Gravity-dominated Collisions: A Model for the Largest Remnant Masses with Treatment for “Hit and Run” and Density Stratification | en_US |
dc.type | Article | en_US |
dc.contributor.department | Univ Arizona, Lunar & Planetary Inst | en_US |
dc.identifier.journal | ASTROPHYSICAL JOURNAL | en_US |
dc.description.note | Open access article | en_US |
dc.description.collectioninformation | This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu. | en_US |
dc.eprint.version | Final published version | en_US |
dc.source.journaltitle | The Astrophysical Journal | |
dc.source.volume | 892 | |
dc.source.issue | 1 | |
dc.source.beginpage | 40 | |
refterms.dateFOA | 2020-07-20T21:49:20Z |