2021
DOI: 10.1007/s10712-021-09681-1
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Fluid Dynamics Experiments for Planetary Interiors

Abstract: Understanding fluid flows in planetary cores and subsurface oceans, as well as their signatures in available observational data (gravity, magnetism, rotation, etc.), is a tremendous interdisciplinary challenge. In particular, it requires understanding the fundamental fluid dynamics involving turbulence and rotation at typical scales well beyond our day-to-day experience. To do so, laboratory experiments are fully complementary to numerical simulations, especially in systematically exploring extreme flow regime… Show more

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Cited by 18 publications
(9 citation statements)
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“…7 Compilation of current approximate pressure-temperature capabilities of static high-pressure, hightemperature experimental equipment Mandea 2008). The theory of liquid convection in fast rotating planetary spherical shells is behind these variations, as also discussed in Le Bars et al (2021). For a fluid shell with a positive temperature gradient imposed between inner and outer core boundary, convection starts as columns outside the tangent cylinder (i.e., Inner Core Boundary, ICB) parallel to the Earth rotation axis (see Fig.…”
Section: Magnetic Field Observations Providing Information On the Corementioning
confidence: 99%
“…7 Compilation of current approximate pressure-temperature capabilities of static high-pressure, hightemperature experimental equipment Mandea 2008). The theory of liquid convection in fast rotating planetary spherical shells is behind these variations, as also discussed in Le Bars et al (2021). For a fluid shell with a positive temperature gradient imposed between inner and outer core boundary, convection starts as columns outside the tangent cylinder (i.e., Inner Core Boundary, ICB) parallel to the Earth rotation axis (see Fig.…”
Section: Magnetic Field Observations Providing Information On the Corementioning
confidence: 99%
“…In regard to Earth, numerical simulations of the geodynamo [3][4][5] established that MHD processes within the Earth are capable of creating a magnetic field similar to the actual geomagnetic field, including reversals of the dominant dipole component. In addition, there have been many laboratory experiments [6], some of which have shown the growth of a self-generated magnetic field, i.e., a dynamo [7][8][9]. Although numerical simulations have been successful in proving the MHD nature of the geodynamo and experiments have shown a dynamo effect, the fundamental MHD origin of the dominant, quasi-steady geomagnetic dipole field still appear to be a theoretical mystery [10].…”
Section: Introductionmentioning
confidence: 99%
“…For planets and moons, it is estimated that EOfalse(1014false), RoOfalse(105false) and PoOfalse(107false) [1]. Such small E are unattainable in laboratory experiments, where the lower limit is EOfalse(106false), and the forcing amplitudes are considerably larger in order to have reasonable signal-to-noise ratios [2,3]. The concept of extracting a portion of the available rotational energy in a rapidly rotating contained body of fluid via low-amplitude parametric forcing and converting it into intense fluid motions via the resonant excitation of inertial waves has a long history [4], and continues to be of great interest [5].…”
Section: Introductionmentioning
confidence: 99%