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Consequences of Tidal Dissipation in a Putative Venusian Ocean
Bangor Univ Menai Bridge, Sch Ocean Sci, Bangor LL59 5AB, Gwynedd, Wales.
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics. NASA, Goddard Inst Space Studies, New York, NY 10025 USA.ORCID iD: 0000-0003-3728-0475
Univ Washington, Dept Astron, Seattle, WA 98195 USA.
2019 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 876, no 2, article id L22Article in journal (Refereed) Published
Abstract [en]

The solar tide in an ancient Venusian ocean is simulated using a dedicated numerical tidal model. Simulations with varying ocean depth and rotational periods ranging from -243 to 64 sidereal Earth days are used to calculate the tidal dissipation rates and associated tidal torque. The results show that the tidal dissipation could have varied by more than 5 orders of magnitude, from 0.001 to 780 GW, depending on rotational period and ocean depth. The associated tidal torque is about 2 orders of magnitude below the present day Venusian atmospheric torque, and could change the Venusian daylength by up to 72 days per million years depending on rotation rate. Consequently, an ocean tide on ancient Venus could have had significant effects on the rotational history of the planet. These calculations have implications for the rotational periods of similarly close-in exoplanetary worlds and the location of the inner edge of the liquid water habitable zone.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD , 2019. Vol. 876, no 2, article id L22
Keywords [en]
planets and satellites: dynamical evolution and stability
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-384066DOI: 10.3847/2041-8213/ab133bISI: 000467116000005OAI: oai:DiVA.org:uu-384066DiVA, id: diva2:1327917
Available from: 2019-06-20 Created: 2019-06-20 Last updated: 2019-06-20Bibliographically approved

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