dc.contributor.author | Antonini, Fabio | |
dc.contributor.author | Capuzzo-Dolcetta, Roberto | |
dc.contributor.author | Merritt, David | |
dc.date.accessioned | 2009-02-25T16:10:32Z | |
dc.date.available | 2009-02-25T16:10:32Z | |
dc.date.issued | 2008-12 | |
dc.identifier.citation | Astronomische Nachrichten 327 (2008) 900-903 | en_US |
dc.identifier.uri | http://hdl.handle.net/1850/8497 | |
dc.description | RIT community members may access full-text via RIT Libraries licensed databases: http://library.rit.edu/databases/ | |
dc.description.abstract | The radial-orbit instability is a collective phenomenon that has heretofore only been observed in spherical systems. We
find that this instability occurs also in triaxial systems, as we checked by performing extensive N-body simulations whose
initial conditions were obtained by sampling a self-consistent triaxial model of a cuspy galaxy composed of luminous
and dark matter. N-body simulations show a time evolution of the galaxy that is not due to the development of chaotic
motions but, rather, to the collective instability induced by an excess of box-like orbits. The instability quickly transforms
such models into a more prolate configuration, with 0.64 < b/a < 0.77 and 0.6 < c/a < 0.7 for the dark halo and
0.64 < b/a < 0.77 and 0.59 < c/a < 0.67 for the luminous matter. Stable triaxial, cuspy galaxies with dark matter
halos are obtained when the contribution of radially-biased orbits to the solution is reduced. These results constitute the
first evidence of the radial-orbit instability in triaxial galaxy models. | en_US |
dc.language.iso | en_US | en_US |
dc.publisher | Wiley InterScience: Astronomische Nachrichten | en_US |
dc.relation.ispartofseries | vol. 327 | en_US |
dc.relation.ispartofseries | no. 9-10 | en_US |
dc.relation.ispartofseries | pps. 900-903 | en_US |
dc.title | An Instability in triaxial stellar systems | en_US |
dc.type | Article | en_US |
dc.identifier.url | http://dx.doi.org/10.1002/asna.200811071 | |