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Bibliografías temáticas / Stellar perturbation theory

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Artículos de revistas

Literatura académica sobre el tema "Stellar perturbation theory"

Autor: Grafiati

Publicado: 22 de febrero de 2023

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Artículos de revistas sobre el tema "Stellar perturbation theory"

1

Magorrian, John. "Stellar dynamics in the periodic cube." Monthly Notices of the Royal Astronomical Society 507, no. 4 (2021): 4840–51. http://dx.doi.org/10.1093/mnras/stab2457.

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ABSTRACT We use the problem of dynamical friction within the periodic cube to illustrate the application of perturbation theory in stellar dynamics, testing its predictions against measurements from N-body simulations. Our development is based on the explicitly time-dependent Volterra integral equation for the cube’s linear response, which avoids the subtleties encountered in analyses based on complex frequency. We obtain an expression for the self-consistent response of the cube to steady stirring by an external perturber. From this, we show how to obtain the familiar Chandrasekhar dynamical

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2

Kolláth, Z., and J. Nuspl. "Resonance Between Pulsation Modes Due to Tidal Perturbation." Symposium - International Astronomical Union 151 (1992): 289–92. http://dx.doi.org/10.1017/s0074180900122314.

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The effect of tidal perturbation to stellar pulsation is a relatively underdeveloped problem in the theory of variable stars. We derive amplitude equations describing the resonances between pulsational modes and orbital motion taking into consideration the rotation of stars as well. In the case of δ Scuti stars the two-mode-tidal resonance was found to be the most powerful effect. If the difference between frequencies of excited and damped mode is close to the orbital frequency, parametric excitation of the damped mode may occur, while the other mode loses energy. We discuss this effect for a

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3

Georgakarakos, Nikolaos, and Siegfried Eggl. "Eccentricity estimates in hierarchical triple systems." Proceedings of the International Astronomical Union 9, S310 (2014): 88–89. http://dx.doi.org/10.1017/s1743921314007923.

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AbstractPerturbation theory in the three body problem has greatly advanced our ability to understand and model a variety of systems ranging from artificial satellites to stars and from extrasolar planets to asteroid-Jupiter interactions. In a series of papers, we developed an analytical technique for estimating the orbital eccentricity of the inner binary in hierarchical triple systems. The method combined the secular theory with calculations of short period terms. The derivation of the short term component was based on an expansion of the rate of change of the Runge-Lenz vector by using first

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4

Famaey, B., G. Monari, A. Siebert, J. B. Fouvry, and J. Binney. "Distribution functions for Galactic disc stellar populations in the presence of non-axisymmetric perturbations." Proceedings of the International Astronomical Union 13, S334 (2017): 195–98. http://dx.doi.org/10.1017/s174392131700672x.

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AbstractThe present-day response of a Galactic disc stellar population to a non-axisymmetric perturbation of the potential, in the form of a bar or spiral arms, can be treated, away from the main resonances, through perturbation theory within the action-angle coordinates of the unperturbed axisymmetric system. The first order moments of such a perturbed distribution function (DF) in the presence of spiral arms give rise to non-zero radial and vertical mean stellar velocities, called breathing modes. Such an Eulerian linearized treatment however diverges at resonances. The Lagrangian approach t

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5

Spurzem, R. "On Gravothermal Instability of Anisotropic Self-Gravitating Gas Spheres: Singular Equilibrium Solution." International Astronomical Union Colloquium 132 (1993): 241–53. http://dx.doi.org/10.1017/s0252921100066136.

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AbstractA reinvestigation of the linear perturbation theory is presented, which examines the hydrostatic readjustment of an isolated self-gravitating gas sphere to a redistribution of energy. The here presented model describes a stellar system by the common equations of gas in hydrostatic equilibrium but with the effect of the anisotropic velocity distribution on the pressure gradient. We take as equilibrium models the singular isothermal solution with and without anisotropy. The total variation of the Boltzmann entropy resulting from a perturbation of the system caused by a redistribution of

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6

Polyachenko, E. V., P. Berczik, A. Just, and I. G. Shukhman. "Simulation of the loss-cone instability in spherical systems – I. Dominating harmonic potential." Monthly Notices of the Royal Astronomical Society 492, no. 1 (2019): 645–50. http://dx.doi.org/10.1093/mnras/stz3544.

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ABSTRACT A new so-called ‘gravitational loss-cone instability’ in stellar systems has recently been investigated theoretically in the framework of linear perturbation theory and proved to be potentially important in understanding the physical processes in centres of galaxies, star clusters, and the Oort Cloud. Using N-body simulations of a toy model, we confirm previous findings for the dominating harmonic potential and go beyond the linear theory. Unlike the well-known instabilities, the new one shows no notable change in the spherical geometry of the cluster, but it significantly accelerates

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7

Malmqvist, Per-Åke. "The RASSCF, RASSI, and CASPT2 Methods Used on Small Molecules of Astrophysical Interest." International Astronomical Union Colloquium 146 (1994): 338–52. http://dx.doi.org/10.1017/s0252921100021448.

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To a quantum chemist with no particular background in astrophysics or astronomy, a brief glance at journals and textbooks in these fields shows at least three areas where computational quantum chemistry has had a valuable impact: Interstellar cloud chemistry; stellar atmosphere modelling; and chemistry in extreme conditions, such as at the surface of a neutron star. The first two uses are particularly suitable, since standard methods are directly applicable.For such problems, good calculations of potential energy as well as expectation values and matrix elements of dipole and other operators a

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8

Yavetz, Tomer D., Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, and Martin D. Weinberg. "Separatrix divergence of stellar streams in galactic potentials." Monthly Notices of the Royal Astronomical Society 501, no. 2 (2020): 1791–802. http://dx.doi.org/10.1093/mnras/staa3687.

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ABSTRACT Flattened axisymmetric galactic potentials are known to host minor orbit families surrounding orbits with commensurable frequencies. The behaviour of orbits that belong to these orbit families is fundamentally different than that of typical orbits with non-commensurable frequencies. We investigate the evolution of stellar streams on orbits near the boundaries between orbit families (separatrices) in a flattened axisymmetric potential. We demonstrate that the separatrix divides these streams into two groups of stars that belong to two different orbit families, and that as a result, the

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9

GEROYANNIS, V. S., and A. G. KATELOUZOS. "NUMERICAL TREATMENT OF HARTLE'S PERTURBATION METHOD FOR DIFFERENTIALLY ROTATING NEUTRON STARS SIMULATED BY GENERAL-RELATIVISTIC POLYTROPIC MODELS." International Journal of Modern Physics C 19, no. 12 (2008): 1863–908. http://dx.doi.org/10.1142/s0129183108013370.

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We compute general-relativistic polytropic models of differentially rotating neutron stars. A brief description of our numerical treatment is given as follows. First, the relativistic Oppenheimer–Volkoff equations of hydrostatic equilibrium are solved for nonrotating models obeying the well-known polytropic equation of state. Then, uniform rotation assumed for such models is treated in the framework of Hartle's perturbation method; thus, corrections to mass and radius, owing to spherical and quadrupole deformations, are calculated. Next, a perturbative approach to the stellar structure up to t

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10

Soufi, F., M. J. Goupil, W. A. Dziembowski, and R. Sienkiewicz. "Consequences of Rapid Rotation on Mode Identification." International Astronomical Union Colloquium 155 (1995): 321–22. http://dx.doi.org/10.1017/s0252921100037301.

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The present work deals with the effect of rotation on the adiabatic oscillation frequencies of stellar models. Here, rotation, as described in a perturbation theory, is said to be rapid in the sense that second order perturbation effects have to be taken into account. Rotation has two second order effects on the oscillation frequencies: departure from equidistance within a given multiplet split by rotation and an overall shift of the multiplet itself. The first effect has been investigated for realistic models of δ Scuti stars in uniform rotation (Dziembowski & Goode, 1992), whereas H. Sai

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