TROVA, Audrey; HURÉ, J.-M.; HERSANT, F.

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Licencia de uso del documento

TROVA, Audrey
FORMATION STELLAIRE 2011

HURÉ, J.-M.
FORMATION STELLAIRE 2011

HERSANT, F.
FORMATION STELLAIRE 2011

Idioma

Communication dans un congrès

Este ítem está publicado en

SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem, R. Samadi and D. Valls-Gabaud, pp.685-688, 2011, SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem, R. Samadi and D. Valls-Gabaud, pp.685-688, 2011, 2011, Paris. 2011-12p. 685-688

Resumen en inglés

The determination of the gravitational potential inside celestial bodies (rotating stars, discs, planets, asteroids) is a common challenge in numerical Astrophysics. Under axial symmetry, the potential is classically found from a two-dimensional integral over the body's meridional cross-section. Because it involves an improper integral, high accuracy is generally difficult to reach. We have discovered that, for homogeneous bodies, the singular Green kernel can be converted into a regular kernel by direct analytical integration. This new kernel, easily managed with standard techniques, opens interesting horizons, not only for numerical calculus but also to generate approximations, in particular for geometrically thin discs and rings.< Leer menos

Palabras clave en inglés

Gravitation

Methods: analytical

Celestial mechanics

Orígen

Importado de Hal

Centros de investigación

Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804