scholarly journals Periodic and quasi-periodic attractors for the spin–orbit evolution of Mercury with a realistic tidal torque

2017 ◽  
Vol 469 (1) ◽  
pp. 127-150 ◽  
Author(s):  
Michele Bartuccelli ◽  
Jonathan Deane ◽  
Guido Gentile
Keyword(s):  
Spin Orbit ◽  
Tidal Torque ◽  
Orbit Evolution ◽  
Periodic Attractors

scholarly journals Effects of magnetic braking and tidal friction on hot Jupiters

2008 ◽  
Vol 4 (S259) ◽  
pp. 295-302
Author(s):  
Adrian J. Barker ◽  
Gordon I. Ogilvie
Keyword(s):  
Evolution Equations ◽  
Phase Plane Analysis ◽  
Spin Orbit ◽  
Tidal Evolution ◽  
Tidal Friction ◽  
Hot Jupiters ◽  
Secular Evolution ◽  
Orbit Evolution ◽  
Short Period ◽  
Magnetic Braking

AbstractTidal friction is thought to be important in determining the long-term spin-orbit evolution of short-period extrasolar planetary systems. Using a simple model of the orbit-averaged effects of tidal friction (Eggleton et al. 1998), we analyse the effects of the inclusion of stellar magnetic braking on the evolution of such systems. A phase-plane analysis of a simplified system of equations, including only the stellar tide together with a model of the braking torque proposed by Verbunt & Zwaan (1981), is presented. The inclusion of stellar magnetic braking is found to be extremely important in determining the secular evolution of such systems, and its neglect results in a very different orbital history. We then show the results of numerical integrations of the full tidal evolution equations, using the misaligned spin and orbit of the XO-3 system as an example, to study the accuracy of simple timescale estimates of tidal evolution. We find that it is essential to consider coupled evolution of the orbit and the stellar spin in order to model the behaviour accurately. In addition, we find that for typical Hot Jupiters the stellar spin-orbit alignment timescale is of the same order as the inspiral time, which tells us that if a planet is observed to be aligned, then it probably formed coplanar. This reinforces the importance of Rossiter-McLaughlin effect observations in determining the degree of spin-orbit alignment in transiting systems.

scholarly journals Spin-orbit evolution of the GJ 667C system: the effect of composition and other planets’ perturbations

2016 ◽  
Vol 463 (2) ◽  
pp. 1592-1604 ◽  
Author(s):  
P. A. Cuartas-Restrepo ◽  
M. Melita ◽  
J. I. Zuluaga ◽  
B. Portilla-Revelo ◽  
M. Sucerquia ◽  
...  
Keyword(s):  
Spin Orbit ◽  
Orbit Evolution

scholarly journals Spin–orbit evolution of Mercury revisited

Icarus ◽  
2014 ◽  
Vol 241 ◽  
pp. 26-44 ◽  
Author(s):  
Benoît Noyelles ◽  
Julien Frouard ◽  
Valeri V. Makarov ◽  
Michael Efroimsky
Keyword(s):  
Spin Orbit ◽  
Orbit Evolution

scholarly journals Spin-orbit coupling for close-in planets

2019 ◽  
Vol 630 ◽  
pp. A102 ◽  
Author(s):  
Alexandre C. M. Correia ◽  
Jean-Baptiste Delisle
Keyword(s):  
Spin Dynamics ◽  
Orbit Coupling ◽  
New Method ◽  
Spin Orbit Coupling ◽  
Spin Orbit ◽  
Circular Orbits ◽  
Tidal Torque ◽  
Orbital Perturbations ◽  
Multi Body ◽  
Orbit Problem

We study the spin evolution of close-in planets in multi-body systems and present a very general formulation of the spin-orbit problem. This includes a simple way to probe the spin dynamics from the orbital perturbations, a new method for computing forced librations and tidal deformation, and general expressions for the tidal torque and capture probabilities in resonance. We show that planet–planet perturbations can drive the spin of Earth-size planets into asynchronous or chaotic states, even for nearly circular orbits. We apply our results to Mercury and to the KOI-1599 system of two super-Earths in a 3/2 mean motion resonance.

scholarly journals Spin‐Orbit Evolution of Short‐Period Planets

2004 ◽  
Vol 610 (1) ◽  
pp. 464-476 ◽  
Author(s):  
Ian Dobbs‐Dixon ◽  
D. N. C. Lin ◽  
Rosemary A. Mardling
Keyword(s):  
Spin Orbit ◽  
Orbit Evolution ◽  
Short Period

Spinning stars and cosmic recycling

2019 ◽  
pp. 105-124
Author(s):  
Nils Andersson
Keyword(s):  
Simple Model ◽  
Gravitational Wave ◽  
Crab Pulsar ◽  
Spin Orbit ◽  
Rotating Stars ◽  
Orbit Evolution

This chapter considers the relevance of rotating stars as gravitational-wave sources, introducing the notion of a deformed spinning star and estimating the associated gravitational-wave strength through the quadrupole formula. The estimates are compared to the observed spin-down rate for the Crab Pulsar, providing a first idea of how faint these signals are likely to be. Additional physics that must be considered for accreting systems is introduced and a simple model for the spin–orbit evolution of such systems is outlined.

The E-ring: interactions with plasma and implications for its evolution

1984 ◽  
Vol 75 ◽  
pp. 599-602
Author(s):  
T.V. Johnson ◽  
G.E. Morfill ◽  
E. Grun
Keyword(s):  
Time Scale ◽  
Particle Density ◽  
High Energy ◽  
Particle Removal ◽  
Density Region ◽  
Drag Forces ◽  
Orbit Evolution ◽  
History Of ◽  
Ring Particle ◽  
Ring Material

A number of lines of evidence suggest that the particles making up the E-ring are small, on the order of a few microns or less in size (Terrile and Tokunaga, 1980, BAAS; Pang et al., 1982 Saturn meeting; Tucson, AZ). This suggests that a variety of electromagnetic and plasma affects may be important in considering the history of such particles. We have shown (Morfill et al., 1982, J. Geophys. Res., in press) that plasma drags forces from the corotating plasma will rapidly evolve E-ring particle orbits to increasing distance from Saturn until a point is reached where radiation drag forces acting to decrease orbital radius balance this outward acceleration. This occurs at approximately Rhea's orbit, although the exact value is subject to many uncertainties. The time scale for plasma drag to move particles from Enceladus' orbit to the outer E-ring is ~104yr. A variety of effects also act to remove particles, primarily sputtering by both high energy charged particles (Cheng et al., 1982, J. Geophys. Res., in press) and corotating plasma (Morfill et al., 1982). The time scale for sputtering away one micron particles is also short, 102 - 10 yrs. Thus the detailed particle density profile in the E-ring is set by a competition between orbit evolution and particle removal. The high density region near Enceladus' orbit may result from the sputtering yeild of corotating ions being less than unity at this radius (e.g. Eviatar et al., 1982, Saturn meeting). In any case, an active source of E-ring material is required if the feature is not very ephemeral - Enceladus itself, with its geologically recent surface, appears still to be the best candidate for the ultimate source of E-ring material.

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