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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 article, the authors used the semi-empirical atmospheric modeling method to obtain the chro-mospheric temperature, pressure, density and magnetic field distribution versus height in the K2 primary component of the RS CVn binary system HR 7428.
Abstract: In this work we use the semi-empirical atmospheric modeling method to obtain the chro-mospheric temperature, pressure, density and magnetic field distribution versus height in the K2 primary component of the RS CVn binary system HR 7428. While temperature, pressure, density are the standard output of the semi-empirical modeling technique, the chromospheric magnetic field estimation versus height comes from considering the possibility of not im-posing hydrostatic equilibrium in the semi-empirical computation. The stability of the best non-hydrostatic equilibrium model, implies the presence of an additive (toward the center of the star) pressure, that decreases in strength from the base of the chromosphere toward the outer layers. Interpreting the additive pressure as magnetic pressure we estimated a magnetic field intensity of about 500 gauss at the base of the chromosphere.
2 citations
26 Oct 2005
2 citations
TL;DR: In this article, the equations of motion, of continuity, of vorticity and of heat transfer are transformed from coordinates (x, y, z) to coordinates without the use of the hydrostatic equation in the vertical.
Abstract: The equations of motion, of continuity, of vorticity and of heat-transfer are transformed from coordinates (x, y, z) to coordinates (x, y, p) without the use of the hydrostatic equation in the vertical. An approximation based on the empirical fact that the isobaric surfaces are slightly inclined to the horizontal together with the use of dimensionless variables, gives the hydrostatic equation and simplifies the fundamental equations by the rejection of many of their terms. Thereafter definitions of certain types of geostrophic and nongeostrophic motions lead, respectively, to (a) Rossby's potential-vorticity equation; (b) the development and thickness-patterns theory of R. C. Sutcliffe, which is discussed in detail; and (c) J. G. Charney's (1949) treatment of the equivalent barotropic atmosphere. These models of atmospheric motions are compared and contrasted. DOI: 10.1111/j.2153-3490.1952.tb00984.x
2 citations
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TL;DR: In this paper, a class of relativistic solutions with anisotropic fluid for compact stars in hydrostatic equilibrium is presented, and the interior space-time geometry considered here for compact objects are described by parameters namely, $\lambda$, $k, $A$, $R$ and $n$.
Abstract: We present a class of new relativistic solutions with anisotropic fluid for compact stars in hydrostatic equilibrium. The interior space-time geometry considered here for compact objects are described by parameters namely, $\lambda$, $k$, $A$, $R$ and $n$. The values of the geometrical parameters are determined here for obtaining a class of physically viable stellar models. The energy-density, radial pressure and tangential pressure are finite and positive inside the anisotropic stars. Considering some stars of known mass we present stellar models which describe compact astrophysical objects with nuclear density.
2 citations
TL;DR: In this paper, exact solutions of the following theoretical problem are presented: a plane atmosphere is in hydrostatic equilibrium with a uniform gravity, and the ideal gas law is assumed Heat is generated everywhere at a rate proportional to the local density.
Abstract: Exact solutions of the following theoretical problem are presented: A plane atmosphere is in hydrostatic equilibrium with a uniform gravity The ideal gas law is assumed Heat is generated everywhere at a rate proportional to the local density The atmosphere is maintained in a steady state through cooling by thermal conduction and radiation This problem is reducible to quadratures for a thermal conductivity which is an arbitrary, but prescribed, function of the temperature, and for a radiative loss which is expressible as the product of the density and an arbitrary, but prescribed, function of the pressure The analysis is carried out for the case of power law thermal conductivity, and a radiative loss proportional to the square of the density and to the first power of the temperature The radiative cooling function adopted here has the basic mathematical form for an optically thin medium The solutions reproduce the macroscopic ordering of a hot 'corona' separated from a 'photosphere' by a layer of temperature minimum The analytic solutions allow direct illustration of the interplay between steady energy transport and the requirements of hydrostatic equilibrium
2 citations