Consequences of Tidal Dissipation in a Putative Venusian Ocean

J. A. Mattias Green; Michael J Way; Rory Barnes

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 minus 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 gigawatts (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.

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20190025326

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Goddard Space Flight Center

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Reprint (Version printed in journal)

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Date Acquired

May 23, 2019

Publication Date

May 6, 2019

Publication Information

Publication: Astrophysical Journal Letters

Publisher: American Astronomical Society

Volume: 876

Issue: 2

Issue Publication Date: May 10, 2019

ISSN: 2041-8205

e-ISSN: 2041-8213

DOI: 10.3847/2041-8213/ab133b

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Public

Use by or on behalf of the US Gov. Permitted.

Technical Review

Professional Review

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