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Hydrostatic equilibrium

About: Hydrostatic equilibrium is a research topic. Over the lifetime, 2451 publications have been published within this topic receiving 62172 citations.


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TL;DR: In this paper, it is shown that nonhydrostatic effects give rise to pressure distributions which counter hydrostatic pressure gradients in the fluid, and these effects are largest in sinking plume events and can be substantial when plumes are free to sink to depths of 100 m.
Abstract: The distribution of dense brine under leads in sea ice is associated with convective sinking of individual plumes and near-surface mixing associated with ice-water momentum flux. The processes have been studied in the recent Lead Experiment (LeadEx) field program and previously modeled using a two-dimensional hydrostatic numerical model. In this study these processes are reexamined using a nonhydrostatic model. It is shown that nonhydrostatic effects give rise to pressure distributions which counter hydrostatic pressure gradients in the fluid. These effects are largest in sinking plume events and can be substantial when plumes are free to sink to depths of 100 m. In the presence of the Arctic halocline (typically at 30–40 m), however, vertical accelerations of convective plumes are limited spatially and temporally, and nonhydrostatic effects are relatively small. It is the purpose of this paper to demonstrate that for realistic Arctic stratification, convective circulations under leads in sea ice are predominantly hydrostatic.

27 citations

Journal ArticleDOI
TL;DR: Dehant et al. as mentioned in this paper evaluated the atmospheric pressure effects on the Earth's Free Core Nutation (FCN) and some forced nutations and evaluated numerically from the global pressure field provided by the European Center for Medium Range Weather Forecast (ECMWF).

27 citations

Journal ArticleDOI
TL;DR: In this article, a d-dimensional spherically symmetric line element in the context of the Einstein-centric gravity was considered and the hydrostatic equilibrium equation of stars was obtained by using the lowest-order constrained variational (LOCV) method with the AV18 potential.
Abstract: Regarding a d-dimensional spherically symmetric line element in the context of Einstein- $ \Lambda$ gravity, the hydrostatic equilibrium equation of stars is obtained. Then, by using the lowest-order constrained variational (LOCV) method with the AV18 potential and employing microscopic many-body calculations in the modern equation of state, the structure properties of neutron stars are investigated. Regardless of the cosmological point of view and considering arbitrary positive and negative values of the cosmological constant, the maximum mass of the neutron stars and their corresponding radius in 4 dimensions are computed. The results show that there is an upper limit for the maximum mass of a neutron star for a positive cosmological constant ( $ M_{max} \leq 1.68M_{\odot}$ ). On the other hand, it is shown that the Einstein gravity cannot explain the structure of neutron star with negative $ \Lambda$ . Other properties of neutron stars such as the Schwarzschild radius, average density, compactness and Buchdahl-Bondi bound are studied. In addition, by using the Buchdahl-Bondi bound for neutron stars, stability of these stars is investigated. Finally, the dynamical stability is investigated and it is shown that the neutron stars follow the dynamical stability in this gravity.

27 citations

Journal ArticleDOI
TL;DR: In this article, the drag produced by 2D orographic gravity waves trapped at a temperature inversion and waves propagating in the stably stratified layer existing above are explicitly calculated using linear theory, for a two-layer atmosphere with neutral static stability near the surface, mimicking a well-mixed boundary layer.
Abstract: The drag produced by 2D orographic gravity waves trapped at a temperature inversion and waves propagating in the stably stratified layer existing above are explicitly calculated using linear theory, for a two-layer atmosphere with neutral static stability near the surface, mimicking a well-mixed boundary layer. For realistic values of the flow parameters, trapped-lee-wave drag, which is given by a closed analytical expression, is comparable to propagating-wave drag, especially in moderately to strongly nonhydrostatic conditions. In resonant flow, both drag components substantially exceed the single-layer hydrostatic drag estimate used in most parameterization schemes. Both drag components are optimally amplified for a relatively low-level inversion and Froude numbers Fr ≈ 1. While propagating-wave drag is maximized for approximately hydrostatic flow, trapped-lee-wave drag is maximized for l2a = O(1) (where l2 is the Scorer parameter in the stable layer and a is the mountain width). This roughly ha...

27 citations

Journal ArticleDOI
TL;DR: In this article, a series of numerical models for radiatively driven, quasi-static winds from the surfaces of hot neutron stars are constructed for the integration of the fluid equations in the vicinity of the sonic point and an improved treatment of radiative transfer is developed that is appropriate to the exotic physical conditions encountered in the models.
Abstract: A series of numerical models is constructed for radiatively driven, quasi-static winds from the surfaces of hot neutron stars. A mathematical technique is devised that in many cases facilitates the integration of the fluid equations in the vicinity of the sonic point, and an improved treatment of radiative transfer is developed that is appropriate to the exotic physical conditions encountered in the models. Boundary conditions which are more realistic than previous ones are used in these models. In agreement with earlier studies, it is found that radiatively driven winds are likely to be directly relevant to the existence of precursors in fast X-ray transients and to apparent radius variations during the course of some type I bursts, and that the presence of such a wind should prevent the bolometric luminosity of a neutron star from exceeding the Eddington limit by more than a small fractional amount. Formulas describing the wind models are presented which are usable as boundary conditions for calculations of the evolution of the deeper, hydrostatic layers of a neutron-star envelope.

27 citations


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Performance
Metrics
No. of papers in the topic in previous years
YearPapers
2023282
2022708
202167
202089
201998
201893