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

Result code in 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>
Result on the web
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DOI - Digital Object Identifier
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Result language
angličtina
Original language name
The thermal and orbital evolution of Enceladus: observational constraints and models
Original language description
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 "resonance-locking" 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.
Czech name
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Czech description
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Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year
2018
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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