Dynamic reorientation of tidally locked bodies: Application to Pluto

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10466955" target="_blank" >RIV/00216208:11320/23:10466955 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=QD4jC16wt8" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=QD4jC16wt8</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.epsl.2023.118270" target="_blank" >10.1016/j.epsl.2023.118270</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Dynamic reorientation of tidally locked bodies: Application to Pluto

Popis výsledku v původním jazyce

Planets and moons reorient in space due to mass redistribution associated with various types of internal and external processes. While the equilibrium orientation of a tidally locked body is well understood, much less explored are the dynamics of the reorientation process (or true polar wander, TPW, used here for the motion of either the rotation or the tidal pole). TPW dynamics can be non-trivial and are important for predicting the patterns of TPW-induced surface fractures, as well as for assessing whether enough time has passed for the equilibrium orientation to be reached. The only existing and relatively complex numerical method for an accurate evaluation of the reorientation dynamics of a tidally locked body was described in a series of papers by Hu et al. (2017a,b, 2019). Here we demonstrate that an identical solution can be obtained with a simpler approach, denoted as o &amp; omega;||mMIA, because during TPW the tidal and the rotation axes closely follow respectively the minor and the major axes of the total, time-evolving inertia tensor of the body. Motivated by the presumed reorientation of Pluto, the use of the o &amp; omega;||mMIA method is illustrated on several test examples. In particular, we vary the load sign and the mass of the host body and analyze whether TPW paths are curved or straight. When tidal forcing is relatively small, the paths of negative anomalies (e.g. basins) towards the rotation pole are highly curved, while positive loads may reach the sub-or anti-host point straightforwardly. The obtained behavior is explained by the relative timing of longitudinal and latitudinal reorientation. Our results suggest that the Sputnik Planitia basin cannot be a negative anomaly at present day, and that the remnant figure of Pluto must have formed prior to the reorientation. Finally, the presented method is complemented with an energy balance that can be used to test the numerical solution and to quantify the changes in orbital distance due to TPW. A new release of the custom written code LIOUSHELL that is used to perform the simulations is made freely available on GitHub.&amp; COPY; 2023 Elsevier B.V. All rights reserved.

Název v anglickém jazyce

Dynamic reorientation of tidally locked bodies: Application to Pluto

Popis výsledku anglicky

Planets and moons reorient in space due to mass redistribution associated with various types of internal and external processes. While the equilibrium orientation of a tidally locked body is well understood, much less explored are the dynamics of the reorientation process (or true polar wander, TPW, used here for the motion of either the rotation or the tidal pole). TPW dynamics can be non-trivial and are important for predicting the patterns of TPW-induced surface fractures, as well as for assessing whether enough time has passed for the equilibrium orientation to be reached. The only existing and relatively complex numerical method for an accurate evaluation of the reorientation dynamics of a tidally locked body was described in a series of papers by Hu et al. (2017a,b, 2019). Here we demonstrate that an identical solution can be obtained with a simpler approach, denoted as o &amp; omega;||mMIA, because during TPW the tidal and the rotation axes closely follow respectively the minor and the major axes of the total, time-evolving inertia tensor of the body. Motivated by the presumed reorientation of Pluto, the use of the o &amp; omega;||mMIA method is illustrated on several test examples. In particular, we vary the load sign and the mass of the host body and analyze whether TPW paths are curved or straight. When tidal forcing is relatively small, the paths of negative anomalies (e.g. basins) towards the rotation pole are highly curved, while positive loads may reach the sub-or anti-host point straightforwardly. The obtained behavior is explained by the relative timing of longitudinal and latitudinal reorientation. Our results suggest that the Sputnik Planitia basin cannot be a negative anomaly at present day, and that the remnant figure of Pluto must have formed prior to the reorientation. Finally, the presented method is complemented with an energy balance that can be used to test the numerical solution and to quantify the changes in orbital distance due to TPW. A new release of the custom written code LIOUSHELL that is used to perform the simulations is made freely available on GitHub.&amp; COPY; 2023 Elsevier B.V. All rights reserved.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10500 - Earth and related environmental sciences

Projekt

<a href="/cs/project/GA22-20388S" target="_blank" >GA22-20388S: Vývoj vnějších slupek ledových měsíců z pohledu numerického modelování</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2023

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Earth and Planetary Science Letters

ISSN

0012-821X

e-ISSN

1385-013X

Svazek periodika

617

Číslo periodika v rámci svazku

Neuveden

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

13

Strana od-do

118270

Kód UT WoS článku

001032046400001

EID výsledku v databázi Scopus

2-s2.0-85163211205