Beckman, J. E.; Varela, A. M.; Cepa, J.
Referencia bibliográfica
(IAU, European Regional Astronomy Meeting, 11th, La Laguna, Spain, July 3-8, 1989) Astrophysics and Space Science (ISSN 0004-640X), vol. 170, no. 1-2, Aug. 1990, p. 327-335.
Fecha de publicación:
8
1990
Número de citas
1
Número de citas referidas
1
Descripción
An aspect of the missing mass problem in galaxies, not easy to address,
is whether the dynamical mass distribution is spherical or greatly
flattened, following the light. Rotation curves of spirals out of the
plane of the disk cannot, by definition, be measured. A way around this
problem might be to use satellite galaxies orbiting within a few
Holmberg radii of their parents. In this paper, the difficulties implied
in using a satellite are addressed in this way: to what extent is it
possible to solve uniquely for its orbital parameters? A practical set
of solutions which can constrain an orbit is derived using the tidal
radius of the satellite to scale the gravitational pull of the parent.
Although data of the quality needed exist as yet for very few systems,
it is shown, using M31, NGC 128, and NGC 1023 and their respective
satellites, how the dynamics of the interactions can be explored.