Tidal insights into rocky and icy bodies: an introduction and overview

Bagheri, Amirhossein; Efroimsky, Michael; Castillo‐Rogez, Julie; Goossens, Sander; Plesa, Ana‐Catalina; Rambaux, N.; Rhoden, A. R.; Walterová, Michaela; Khan, Amir; Giardini, Domenico

doi:10.1016/bs.agph.2022.07.004

Cited by 26 publications

(16 citation statements)

References 313 publications

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“…To fix this flaw, a more detailed model by Sundberg and Cooper should be employed. A simple review on the topic is available in Section 3 of Walterova et al (2022) and in Section 2 of Bagheri et al (2022).…”

Section: Appendix A: Comparing the Roche Radius And The Synchronous V...mentioning

confidence: 99%

Pathways of Survival of Exomoons and Inner Exoplanets

Makarov¹,

Efroimsky²

2023

Preprint

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Context. It is conceivable that a few thousand confirmed exoplanets initially harboured satellites similar to the moons of the Solar System or larger. We ask the question of whether some of them have survived over the aeons of dynamical evolution to the present day. The dynamical conditions are harsh for exomoons in such systems because of the greater influence of the host star and of the tidal torque it exerts on the planet. Aims. We investigate the stability niches of exomoons around hundreds of innermost exoplanets for which the needed parameters are known today, and we determine the conditions of these moons' long-term survival. General lower and upper bounds on the exomoon survival niches are derived for orbital separations, periods, and masses. Methods. The fate of an exomoon residing in a stability niche depends on the initial relative rate of the planet's rotation and on the ability of the moon to synchronise the planet by overpowering the tidal action from the star. State-of-the-art models of tidal dissipation and secular orbital evolution are applied to a large sample of known exoplanet systems, which have the required estimated physical parameters.Results. We show that in some plausible scenarios, exomoons can prevent close exoplanets from spiralling into their host stars, thus extending these planets' lifetimes. This is achieved when exomoons synchronise the rotation of their parent planets, overpowering the tidal action from the stars. Conclusions. Massive moons are more likely to survive and help their host planets maintain a high rotation rate (higher than these planets' mean motion).

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Section: Appendix A: Comparing the Roche Radius And The Synchronous V...mentioning

confidence: 99%

Pathways of Survival of Exomoons and Inner Exoplanets

Makarov¹,

Efroimsky²

2023

Preprint

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“…While other rheological models exist and have been applied to calculate the tidal deformation of Mars and other rocky planets, the advantange of the Andrade model is the small number of parameters it requires for the calculations (Castillo-Rogez et al, 2011;Efroimsky, 2012). A detailed review of the theory of viscoelasticity and tidal response, as well as their application to constrain the interior structure of Mercury, Venus, Mars, the Moon, and icy satellites is given in Chapter 5 (Bagheri et al, 2022).…”

Section: Symbolmentioning

confidence: 99%

Interior Dynamics and Thermal Evolution of Mars -- a Geodynamic Perspective

Plesa¹,

Wieczorek²,

Knapmeyer³

et al. 2022

Preprint

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Over the past decades, global geodynamical models have been used to investigate the thermal evolution of terrestrial planets. With the increase of computational power and improvement of numerical techniques, these models have become more complex, and simulations are now able to use a high resolution 3D spherical shell geometry and to account for strongly varying viscosity, as appropriate for mantle materials. In this study we review global 3D geodynamic models that have been used to study the thermal evolution and interior dynamics of Mars. We discuss how these models can be combined with local and global observations to constrain the planet's thermal history. In particular, we use the recent InSight estimates of the crustal thickness, upper mantle structure, and core size to show how these constraints can be combined with 3D geodynamic models to improve our understanding of the interior dynamics, present-day thermal state and temperature variations in the interior of Mars. Our results show that the crustal thickness variations control the surface heat flow and the elastic thickness pattern, as well as the location of melting zones in the present-day martian mantle. The lithospheric temperature and the seismic velocities pattern in the shallow mantle reflect the crustal thickness pattern. The large size of the martian core leads to a smaller scale convection pattern in the mantle than previously suggested. Strong mantle plumes that produce melt up to recent times become focused in Tharsis and Elysium, while weaker plumes are distributed throughout the mantle. The thickness of the seismogenic layer, where seismic events can occur, can be used to discriminate between geodynamic models, if the source depth and location of seismic events is known. Furthermore model predictions of present-day martian seismicity can be compared to the values measured by InSight. Future models need to consider recent estimates from the presentday elastic lithosphere thickness at the north pole of Mars, the effects of lateral variations of seismic velocities on waves propagation through the mantle and lithosphere, and to test the spatial distribution of seismicity by comparing model predictions to observations.

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“…Since the discovery of the first exoplanet by Mayor & Queloz (1995) over 5000 exoplanets and almost 4000 exoplanetary systems have been identified and cataloged, hence it is becoming necessary to consider tidal interactions in exoplanetary systems. The tidal response of a planet depends on the timescale of the perturbation and on the rheological properties of its interior (i.e., elasticity, density, and viscosity) (Bagheri et al 2022). Many moons and planets within the solar system exhibit a stratified internal structure, as confirmed by seismic and moment of inertia data.…”

Section: Introductionmentioning

confidence: 95%

Equivalence between simple multilayered and homogeneous laboratory-based rheological models in planetary science

Gevorgyan¹,

Matsuyama²,

Ragazzo³

2023

Preprint

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The main propose of this work is to investigate under which circumstances the tidal response of a stratified body can be approximated by that of a homogeneous body. We show that any multilayered body can be approximated by a homogeneous body, with the same dissipation of tidal energy as a function of the excitation frequency, as long as the rheology of the homogeneous model is sufficiently complex. Moreover we provide a straightforward recipe to associate the aforementioned homogeneous rheology to a given stratified body. These results highlight the fact that the two models cannot be distinguished from each other only by the measurement of the second degree tidal Love number and quality factor, and that we do not need the complexity of the multilayer planet model in order to estimate its tidal dissipation.

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Tidal insights into rocky and icy bodies: an introduction and overview

Cited by 26 publications

References 313 publications

Pathways of Survival of Exomoons and Inner Exoplanets

Pathways of Survival of Exomoons and Inner Exoplanets

Interior Dynamics and Thermal Evolution of Mars -- a Geodynamic Perspective

Equivalence between simple multilayered and homogeneous laboratory-based rheological models in planetary science

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