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Tidal dissipation in Enceladus' uneven, fractured ice shell

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F19%3A10403990" target="_blank" >RIV/00216208:11320/19:10403990 - isvavai.cz</a>

  • Result on the web

    <a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=vopI3Jf2ww" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=vopI3Jf2ww</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.1016/j.icarus.2019.02.012" target="_blank" >10.1016/j.icarus.2019.02.012</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    Tidal dissipation in Enceladus' uneven, fractured ice shell

  • Original language description

    Analysis of Enceladus&apos; gravity, topography and libration data suggests that the thickness of the ice crust significantly varies, which may have important consequences for the heat transfer across and the tidal dissipation within the ice shell. Understanding these processes is a critical prerequisite for analyzing Enceladus&apos; thermal evolution and assessing the long-term stability of its subsurface ocean. Here, we investigate the impact of ice shell thickness variations on the tidal deformation of the moon and the associated heat production using a finite element model that includes faults (&quot;tiger stripes&quot;) in the south polar region (SPR). Since the tidal deformation and the thermal structure of the ice shell are coupled through temperature and deviatoric stress, we simultaneously solve the equations governing the anelastic deformation of ice and also equations which model conductive heat transfer in the ice shell. We find that tidal heating is concentrated in a narrow low viscosity zone near the base of the ice shell and along faults. Outside the SPR, the thickness of this zone is about 1/10 of the local ice thickness and the associated volumetric heating is less than or similar to 10(-6) W/m(3), corresponding to less than 1 GW of dissipated power. In the SPR, the tidal effects are enhanced by the combined action of faults and ice shell thinning. Although the volumetric heating in this relatively small region may be larger than 10(-4) W/m(3), the total heat production in this region does not exceed 1.1 GW. Our computations show that tidal heating in the ice shell can explain only a small fraction of Enceladus&apos; heat production derived from astrometric observations, implying that Enceladus&apos; heat engine is powered by dissipation in the core or in the ocean.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • OECD FORD branch

    10500 - Earth and related environmental sciences

Result continuities

  • Project

  • Continuities

    I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Others

  • Publication year

    2019

  • Confidentiality

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

Data specific for result type

  • Name of the periodical

    Icarus

  • ISSN

    0019-1035

  • e-ISSN

  • Volume of the periodical

    328

  • Issue of the periodical within the volume

    2019

  • Country of publishing house

    US - UNITED STATES

  • Number of pages

    14

  • Pages from-to

    218-231

  • UT code for WoS article

    000469159500018

  • EID of the result in the Scopus database

    2-s2.0-85063763483