Atmospheric Tides

Haurwitz, B.

doi:10.1126/science.144.3625.1415

Cited by 18 publications

(7 citation statements)

References 13 publications

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“…The yearly world-wide average (Haurwitz 1964) of the main atmospheric tides S ( p ) in the atmospheric pressure is when translated into the notation of this paper. The numerical coefficients are in millibars.…”

Section: Atmospheric Tidal Perturbationsmentioning

confidence: 99%

A Satellite Determination of Tidal Parameters and Earth Deceleration

Newton

2010

Geophysical Journal of the Royal Astronomical Society

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This paper uses perturbations in the inclination and in the longitude of the node for four nearly polar satellites to find values of the tidal number k and of the phases for the lunar and solar semi-diurnal tides. In order to obtain the desired accuracy, it was necessary to include the following perturbations in the analysis: (1) differences between UT2c and UTI, (2) the motions of the true coordinate systems of date, including the rotation of the ecliptic, (3) atmospheric drag, (4) radiation pressure, including radiation scattered or emitted by the satellite and including radiation scattered by the Earth as well as direct sunlight, (5) the atmospheric tide, (6) the gravitational perturbations produced by the Sun and Moon, and (7) the perturbations due to the zonal gravity harmonics. For many of these, existing perturbation procedures are not accurate enough, and new methods were devised. The new methods are described. By-products of the perturbation analysis include a small change in the method of inferring wind velocities from orbital data at altitudes around 600 km, and a substantial change in the value of the estimated torque due to the atmospheric tide.The value found for the ratio of lunar to solar tida1 friction torques is considerably greater than that given by any existing model, but is closer to the value generally given for linear friction than to that for non-linear friction. This does not imply that the friction is linear. It is shown that the relation between the torque ratio and the type of friction depends upon an unknown parameter of the oceans. Over a large range of this parameter, which includes plausible values, the ratio of the friction torques is independent of the law of friction.The value found for k is 0.336 f 0-028. The deceleration of the Earth's rotation due to the combination of the gravitational and atmospheric tides is estimated to lie between 16.8 and 21.4 parts in 10" per year. This is lower than other recent estimates and is in better agreement with the value deduced from ancient eclipses.

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Section: Atmospheric Tidal Perturbationsmentioning

confidence: 99%

A Satellite Determination of Tidal Parameters and Earth Deceleration

Newton

2010

Geophysical Journal of the Royal Astronomical Society

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“…In a state of quasi‐hydrostatic equilibrium, the gravitational tide in the ocean and solid Earth and the thermal tide in the atmosphere can be modelled as gravitational and thermal bulges, respectively (see Cartwright 2000 for a historical account). In the case of the Earth, the thermal bulge and the gravitational bulge have opposite phase difference with respect to the Sun (Haurwitz 1964; Cartwright 2000), meaning that the gravitational torques on the thermal bulge and on the gravitational bulge are pointing in opposite directions. Since Venus has a denser atmosphere and receives more solar insolation than the Earth, thermal tides on Venus are expected to be more prominent.…”

Section: Introductionmentioning

confidence: 99%

Diurnal thermal tides in a non-synchronized hot Jupiter

Ogilvie

2009

Monthly Notices of the Royal Astronomical Society

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We perform a linear analysis to investigate the dynamical response of a non‐synchronized hot Jupiter to stellar irradiation. In this work, we consider the diurnal Fourier harmonic of the stellar irradiation acting at the top of a radiative layer of a hot Jupiter with no clouds and winds. In the absence of the Coriolis force, the diurnal thermal forcing can excite internal waves propagating into the planet's interior when the thermal forcing period is longer than the sound crossing time of the planet's surface. When the Coriolis effect is taken into consideration, the latitude‐dependent stellar heating can excite weak internal waves (g modes) and/or strong baroclinic Rossby waves (buoyant r modes) depending on the asynchrony of the planet. When the planet spins faster than its orbital motion (i.e. retrograde thermal forcing), these waves carry negative angular momentum and are damped by radiative loss as they propagate downwards from the upper layer of the radiative zone. As a result, angular momentum is transferred from the lower layer of the radiative zone to the upper layer and generates a vertical shear. We estimate the resulting internal torques for different rotation periods based on the parameters of HD 209458b.

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“…Arras & Socrates 2010). Observations on Earth show that the pressure redistribution is essentially a superposition of two pressure waves: a diurnal tide of small amplitude and a strong semi-diurnal tide (Bartels 1932;Haurwitz 1964;Chapman & Lindzen 1970).…”

Section: Thermal Atmospheric Tidesmentioning

confidence: 99%

“…More precisely, the particles of the atmosphere move from the high-temperature zone (at the sub-solar point) to the low-temperature areas (e.g., Arras & Socrates 2010). Observations on Earth show that the pressure redistribution is essentially a superposition of two pressure waves: a diurnal tide of small amplitude and a strong semi-diurnal tide (Bartels 1932; Haurwitz 1964; Chapman & Lindzen 1970).…”

Section: Equations Of Motionmentioning

confidence: 99%

Spin evolution of Earth-sized exoplanets, including atmospheric tides and core–mantle friction

Cunha

Correia

Laskar

2014

International Journal of Astrobiology

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Planets with masses between 0.1 and 10 M ⊕ are believed to host dense atmospheres. These atmospheres can play an important role on the planet's spin evolution, since thermal atmospheric tides, driven by the host star, may counterbalance gravitational tides. In this work, we study the long-term spin evolution of Earth-sized exoplanets. We generalize previous works by including the effect of eccentric orbits and obliquity. We show that under the effect of tides and core-mantle friction, the obliquity of the planets evolves either to 0°or 180°. The rotation of these planets is also expected to evolve into a very restricted number of equilibrium configurations. In general, none of these equilibria is synchronous with the orbital mean motion. The role of thermal atmospheric tides becomes more important for Earth-sized planets in the habitable zones of their systems; so they cannot be neglected when we search for their potential habitability.

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Atmospheric Tides

Cited by 18 publications

References 13 publications

A Satellite Determination of Tidal Parameters and Earth Deceleration

A Satellite Determination of Tidal Parameters and Earth Deceleration

Diurnal thermal tides in a non-synchronized hot Jupiter

Spin evolution of Earth-sized exoplanets, including atmospheric tides and core–mantle friction

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