Dynamical evolution of the rotation of Venus
type: Item
instance of: scholarly article
title: Dynamical evolution of the rotation of Venus
zbMATH Open document ID: 0662.70015
DOI: 10.1007/BF00117100
author: S. H. Smith
published in: Earth, Moon, and Planets
publication date: 1988-01-01T00:00:00Z
review text: By considering the torque of the bodily tides, the effect of the core- mantle viscous coupling and the torque of the atmospheric tides have been obtained by numerical calculation: the evolution of the spin angular velocity \(\Omega\), and the obliquity \(\beta\) of the Venus are calculated numerically with the step-variable Runge-Kutta method of 7th order; and 7 sets of the probable Cytherean spin evolution have been obtained. It is indicated that the present spin state of Venus is the result of long-term evolution within the reasonable ranges of some disposable parameters. The early spin period is between 7 h to 2 d and the corresponding obliquity is about 90\(\circ \sim 100\circ\). The effects of the torques of body and atmospheric tides and the core-mantle viscous coupling of Venus on its spin angular velocity could nearly cancel out each other about a billion years ago. Therefore, Venus could have been captured in a spin-orbit resonant state by the gravitational torque of the Earth on the permanent deformation part of Venus; and this resonant state has lasted up to the present time.
Mathematics Subject Classification ID: 70F15
zbMATH DE Number: 4083065
zbMATH Keywords: core-mantle viscous coupling
zbMATH Keywords: step-variable Runge-Kutta method
zbMATH Keywords: probable Cytherean spin evolution
MaRDI profile type: Publication
description: scientific article; zbMATH DE number 4083065