dc.creatorWachlin, Felipe Carlos
dc.creatorFerraz-Mello, Sylvio
dc.date1998-07-21
dc.date2022-11-23T15:51:49Z
dc.date.accessioned2023-07-15T05:12:12Z
dc.date.available2023-07-15T05:12:12Z
dc.identifierhttp://sedici.unlp.edu.ar/handle/10915/146269
dc.identifierissn:0035-8711
dc.identifierissn:1365-2966
dc.identifier.urihttps://repositorioslatinoamericanos.uchile.cl/handle/2250/7472471
dc.descriptionWe present an application of the frequency map analysis to an elliptical galaxy which is represented by a generalization of a double-power-law spherical mass model. The density distribution of this model varies as r−γ close to the centre and as r−4 at large radii. We study the case with γ = 1, which is known as the ‘weak-cusp’ model and which represents well the density profile of the ‘core’ galaxies observed by the Hubble Space Telescope. The final objective of our work is to improve our understanding of the dynamics of elliptical galaxies in a similar way to Merritt & Fridman, finding the regions of stochasticity, looking for resonances that might play an important role in sustaining the triaxial morphology, and analysing the diffusion of orbits. To this end, we use the frequency map analysis of Laskar, which has been applied widely in the field of celestial mechanics but which is a relatively new technique in the area of galactic dynamics. Finally, we show some useful features of this method in understanding the global dynamical structure of the system.
dc.descriptionFacultad de Ciencias Astronómicas y Geofísicas
dc.formatapplication/pdf
dc.format22-32
dc.languageen
dc.rightshttp://creativecommons.org/licenses/by-nc-sa/4.0/
dc.rightsCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.subjectCiencias Astronómicas
dc.subjectCelestial mechanics
dc.subjectStellar dynamics
dc.subjectGalaxies: elliptical and lenticular
dc.subjectcD
dc.subjectGalaxies: kinematics and dynamics
dc.titleFrequency map analysis of the orbital structure in elliptical galaxies
dc.typeArticulo
dc.typeArticulo


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