tidal migration
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2021 ◽  
Vol 920 (1) ◽  
pp. L16
Jiayin Dong ◽  
Chelsea X. Huang ◽  
George Zhou ◽  
Rebekah I. Dawson ◽  
Joseph E. Rodriguez ◽  

2021 ◽  
Vol 161 (4) ◽  
pp. 200
Jonathan M. Jackson ◽  
Rebekah I. Dawson ◽  
Andrew Shannon ◽  
Cristobal Petrovich

2020 ◽  
Vol 902 (1) ◽  
pp. L20
Billy Quarles ◽  
Gongjie Li ◽  
Marialis Rosario-Franco

Impact ◽  
2020 ◽  
Vol 2020 (3) ◽  
pp. 32-33
Kusuto Nanjo

The main problems tropical estuaries face are mangrove deforestation and eutrophication that is a result of land development and agriculture fertilization. While these habitat modifications can significantly reduce the fish diversity and production of mangrove ecosystems, the specific mechanisms are not well understood. It is difficult to quantify the fish production in tropical estuaries, because many fish use estuaries at high tide and migrate to other habitats at low tide. Dr Kusuto Nanjo, based at the Department of Applied Aquabiology, National Fisheries University in Japan, focused on resident fish, which utilize estuaries for a certain period of their life history without tidal migration and account for a large proportion of the fish assemblages, as good indicators in assessing the secondary production of mangrove ecosystems. It is hoped that by elucidating this, his team will be able to establish specific conservation measures that protect biodiversity and life within mangrove ecosystems.

2019 ◽  
Vol 157 (4) ◽  
pp. 166
Jonathan M. Jackson ◽  
Rebekah I. Dawson ◽  
Joseph Zalesky

2018 ◽  
Vol 619 ◽  
pp. A133 ◽  
William Polycarpe ◽  
Melaine Saillenfest ◽  
Valéry Lainey ◽  
Alain Vienne ◽  
Benoît Noyelles ◽  

Context. Natural satellite systems present a large variety of orbital configurations in the solar system. While some are clearly the result of known processes, others still have largely unexplained eccentricity and inclination values. Iapetus, the furthest of Saturn’s main satellites, has a still unexplained 3% orbital eccentricity and its orbital plane is tilted with respect to its local Laplace plane (8° of free inclination). On the other hand, astrometric measurements of saturnian moons have revealed high tidal migration rates, corresponding to a quality factor Q of Saturn of around 1600 for the mid-sized icy moons. Aims. We show how a past crossing of the 5:1 mean motion resonance between Titan and Iapetus may be a plausible scenario to explain Iapetus’ orbit. Methods. We have carried out numerical simulations of the resonance crossing using an N-body code as well as using averaged equations of motion. A large span of migration rates were explored for Titan and Iapetus was started on its local Laplace plane (15° with respect to the equatorial plane) with a circular orbit. Results. The resonance crossing can trigger a chaotic evolution of the eccentricity and the inclination of Iapetus. The outcome of the resonance is highly dependent on the migration rate (or equivalently on Q). For a quality factor Q of over around 2000, the chaotic evolution of Iapetus in the resonance leads in most cases to its ejection, while simulations with a quality factor between 100 and 2000 show a departure from the resonance with post-resonant eccentricities spanning from 0 up to 15%, and free inclinations capable of reaching 11°. Usually high inclinations come with high eccentricities but some simulations (less than 1%) show elements compatible with Iapetus’ current orbit Conclusions. In the context of high tidal energy dissipation in Saturn, a quality factor between 100 and 2000 at the frequency of Titan would bring Titan and Iapetus into a 5:1 resonance, which would perturb Iapetus’ eccentricity and inclination to values observed today. Such rapid tidal migration would have avoided Iapetus’ ejection around 40–800 million years ago.

2018 ◽  
Vol 56 (1) ◽  
pp. 175-221 ◽  
Rebekah I. Dawson ◽  
John Asher Johnson

Hot Jupiters were the first exoplanets to be discovered around main sequence stars and astonished us with their close-in orbits. They are a prime example of how exoplanets have challenged our textbook, solar-system inspired story of how planetary systems form and evolve. More than twenty years after the discovery of the first hot Jupiter, there is no consensus on their predominant origin channel. Three classes of hot Jupiter creation hypotheses have been proposed: in situ formation, disk migration, and high-eccentricity tidal migration. Although no origin channel alone satisfactorily explains all the evidence, two major origin channels together plausibly account for properties of hot Jupiters themselves and their connections to other exoplanet populations.

2016 ◽  
Vol 163 (5) ◽  
José Amorim Reis-Filho ◽  
Tommaso Giarrizzo ◽  
Francisco Barros

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