English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Recently, two-component spherical galaxy models have been presented, wherethe stellar profile is described by a Jaffe law, and the total density byanother Jaffe law, or by an $r^{-3}$ law at large radii. We extend these twofamilies to their ellipsoidal axisymmetric counterparts: the JJe and J3emodels. The total and stellar density distributions can have differentflattenings and scale lengths, and the dark matter halo is defined bydifference. First, the analytical conditions required to have a nowherenegative dark matter halo density are derived. The Jeans equations for thestellar component are then solved analytically, in the limit of smallflattenings, also in presence of a central BH. The azimuthal velocitydispersion anisotropy is described by the Satoh $k$-decomposition. Finally, wepresent the analytical formulae for velocity fields near the center and atlarge radii, together with the various terms entering the Virial Theorem. TheJJe and J3e models can be useful in a number of theoretical applications, e.g.to explore the role of the various parameters (flattening, relative scalelengths, mass ratios, rotational support) in determining the behavior of thestellar kinematical fields before performing more time-expensive integrationswith specific galaxy models, to test codes of stellar dynamics, and innumerical simulations of gas flows in galaxies.

Two-component galaxy models with a central BH -- II. The ellipsoidal case