The thermal and orbital evolution of Enceladus: observational constraints and models

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10384961" target="_blank" >RIV/00216208:11320/18:10384961 - isvavai.cz</a>

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

The thermal and orbital evolution of Enceladus: observational constraints and models

Popis výsledku v původním jazyce

Enceladus possesses a global subsurface ocean beneath an ice shell a few tens of km thick, and is observed to be losing heat at a rate of TILDE OPERATOR+D91 10 GW from its south polar region. Two major puzzles are the source of the observed heat, and how the ocean could have been maintained. Tidal dissipation in Enceladus is ultimately controlled by the rate of dissipation within Saturn, parameterized by the factor Qp. AQp of about 2,000 is indicated by astrometric measurements and generates an equilibrium heating rate at Enceladus sufficient to explain the observed heat and maintain an ocean indefinitely if the ice shell is conductive. If constant, this Qp would indicate an age for Enceladus much less than that of the solar system. An alternative, however, termed the &quot;resonance-locking&quot; scenario, is that the effective Qp is time-variable such that the heating rate is almost constant over geological time. This scenario can explain the long-term survival of the ocean and the present-day heat flux without requiring Enceladus to have formed recently.

Název v anglickém jazyce

The thermal and orbital evolution of Enceladus: observational constraints and models

Popis výsledku anglicky

Enceladus possesses a global subsurface ocean beneath an ice shell a few tens of km thick, and is observed to be losing heat at a rate of TILDE OPERATOR+D91 10 GW from its south polar region. Two major puzzles are the source of the observed heat, and how the ocean could have been maintained. Tidal dissipation in Enceladus is ultimately controlled by the rate of dissipation within Saturn, parameterized by the factor Qp. AQp of about 2,000 is indicated by astrometric measurements and generates an equilibrium heating rate at Enceladus sufficient to explain the observed heat and maintain an ocean indefinitely if the ice shell is conductive. If constant, this Qp would indicate an age for Enceladus much less than that of the solar system. An alternative, however, termed the &quot;resonance-locking&quot; scenario, is that the effective Qp is time-variable such that the heating rate is almost constant over geological time. This scenario can explain the long-term survival of the ocean and the present-day heat flux without requiring Enceladus to have formed recently.

Druh

C - Kapitola v odborné knize

CEP obor

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OECD FORD obor

10500 - Earth and related environmental sciences

Projekt

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Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název knihy nebo sborníku

Enceladus and the icy moons of Saturn

ISBN

978-0-8165-3707-5

Počet stran výsledku

16

Strana od-do

79-94

Počet stran knihy

600

Název nakladatele

University of Arizona Press

Místo vydání

USA

Kód UT WoS kapitoly

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