Coupling SPH and thermochemical models of planets

Methodology and example of a Mars-sized body

G. J. Golabek, A. Emsenhuber, M. Jutzi, E. I. Asphaug, T. V. Gerya

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

Giant impacts have been suggested to explain various characteristics of terrestrial planets and their moons. However, so far in most models only the immediate effects of the collisions have been considered, while the long-term interior evolution of the impacted planets was not studied. Here we present a new approach, combining 3-D shock physics collision calculations with 3-D thermochemical interior evolution models.We apply the combined methods to a demonstration example of a giant impact on a Mars-sized body, using typical collisional parameters from previous studies. While the material parameters (equation of state, rheology model) used in the impact simulations can have some effect on the long-term evolution, we find that the impact angle is the most crucial parameter for the resulting spatial distribution of the newly formed crust. The results indicate that a dichotomous crustal pattern can form after a head-on collision, while this is not the case when considering a more likely grazing collision. Our results underline that end-to-end 3-D calculations of the entire process are required to study in the future the effects of large-scale impacts on the evolution of planetary interiors.

Original languageEnglish (US)
JournalIcarus
DOIs
StateAccepted/In press - 2017

Fingerprint

mars
Mars
planets
planet
collision
methodology
collisions
rheology
equation of state
terrestrial planets
Moon
grazing
natural satellites
physics
crust
spatial distribution
crusts
equations of state
shock
simulation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Golabek, G. J., Emsenhuber, A., Jutzi, M., Asphaug, E. I., & Gerya, T. V. (Accepted/In press). Coupling SPH and thermochemical models of planets: Methodology and example of a Mars-sized body. Icarus. https://doi.org/10.1016/j.icarus.2017.10.003

Coupling SPH and thermochemical models of planets : Methodology and example of a Mars-sized body. / Golabek, G. J.; Emsenhuber, A.; Jutzi, M.; Asphaug, E. I.; Gerya, T. V.

In: Icarus, 2017.

Research output: Contribution to journalArticle

Golabek, G. J. ; Emsenhuber, A. ; Jutzi, M. ; Asphaug, E. I. ; Gerya, T. V. / Coupling SPH and thermochemical models of planets : Methodology and example of a Mars-sized body. In: Icarus. 2017.
@article{738d708e4c90415394f6d21b4e9bafc5,
title = "Coupling SPH and thermochemical models of planets: Methodology and example of a Mars-sized body",
abstract = "Giant impacts have been suggested to explain various characteristics of terrestrial planets and their moons. However, so far in most models only the immediate effects of the collisions have been considered, while the long-term interior evolution of the impacted planets was not studied. Here we present a new approach, combining 3-D shock physics collision calculations with 3-D thermochemical interior evolution models.We apply the combined methods to a demonstration example of a giant impact on a Mars-sized body, using typical collisional parameters from previous studies. While the material parameters (equation of state, rheology model) used in the impact simulations can have some effect on the long-term evolution, we find that the impact angle is the most crucial parameter for the resulting spatial distribution of the newly formed crust. The results indicate that a dichotomous crustal pattern can form after a head-on collision, while this is not the case when considering a more likely grazing collision. Our results underline that end-to-end 3-D calculations of the entire process are required to study in the future the effects of large-scale impacts on the evolution of planetary interiors.",
author = "Golabek, {G. J.} and A. Emsenhuber and M. Jutzi and Asphaug, {E. I.} and Gerya, {T. V.}",
year = "2017",
doi = "10.1016/j.icarus.2017.10.003",
language = "English (US)",
journal = "Icarus",
issn = "0019-1035",
publisher = "Academic Press Inc.",

}

TY - JOUR

T1 - Coupling SPH and thermochemical models of planets

T2 - Methodology and example of a Mars-sized body

AU - Golabek, G. J.

AU - Emsenhuber, A.

AU - Jutzi, M.

AU - Asphaug, E. I.

AU - Gerya, T. V.

PY - 2017

Y1 - 2017

N2 - Giant impacts have been suggested to explain various characteristics of terrestrial planets and their moons. However, so far in most models only the immediate effects of the collisions have been considered, while the long-term interior evolution of the impacted planets was not studied. Here we present a new approach, combining 3-D shock physics collision calculations with 3-D thermochemical interior evolution models.We apply the combined methods to a demonstration example of a giant impact on a Mars-sized body, using typical collisional parameters from previous studies. While the material parameters (equation of state, rheology model) used in the impact simulations can have some effect on the long-term evolution, we find that the impact angle is the most crucial parameter for the resulting spatial distribution of the newly formed crust. The results indicate that a dichotomous crustal pattern can form after a head-on collision, while this is not the case when considering a more likely grazing collision. Our results underline that end-to-end 3-D calculations of the entire process are required to study in the future the effects of large-scale impacts on the evolution of planetary interiors.

AB - Giant impacts have been suggested to explain various characteristics of terrestrial planets and their moons. However, so far in most models only the immediate effects of the collisions have been considered, while the long-term interior evolution of the impacted planets was not studied. Here we present a new approach, combining 3-D shock physics collision calculations with 3-D thermochemical interior evolution models.We apply the combined methods to a demonstration example of a giant impact on a Mars-sized body, using typical collisional parameters from previous studies. While the material parameters (equation of state, rheology model) used in the impact simulations can have some effect on the long-term evolution, we find that the impact angle is the most crucial parameter for the resulting spatial distribution of the newly formed crust. The results indicate that a dichotomous crustal pattern can form after a head-on collision, while this is not the case when considering a more likely grazing collision. Our results underline that end-to-end 3-D calculations of the entire process are required to study in the future the effects of large-scale impacts on the evolution of planetary interiors.

UR - http://www.scopus.com/inward/record.url?scp=85031716605&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85031716605&partnerID=8YFLogxK

U2 - 10.1016/j.icarus.2017.10.003

DO - 10.1016/j.icarus.2017.10.003

M3 - Article

JO - Icarus

JF - Icarus

SN - 0019-1035

ER -