Radial-orbit instability in modified Newtonian dynamics

Details Radial-orbit instability in modified Newtonian dynamics Radial-orbit instability in modified Newtonian dynamics

2011-03-02

arxiv.org/abs/1103.0394v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

9 pages, 4 figures, accepted for publication in MNRAS

Scientific paper

The stability of radially anisotropic spherical stellar systems in modified Newtonian dynamics (MOND) is explored by means of numerical simulations performed with the N-body code N-MODY. We find that Osipkov-Merritt MOND models require for stability larger minimum anisotropy radius than equivalent Newtonian systems (ENSs) with dark matter, and also than purely baryonic Newtonian models with the same density profile. The maximum value for stability of the Fridman-Polyachenko-Shukhman parameter in MOND models is lower than in ENSs, but higher than in Newtonian models with no dark matter. We conclude that MOND systems are substantially more prone to radial-orbit instability than ENSs with dark matter, while they are able to support a larger amount of kinetic energy stored in radial orbits than purely baryonic Newtonian systems. An explanation of these results is attempted, and their relevance to the MOND interpretation of the observed kinematics of globular clusters, dwarf spheroidal and elliptical galaxies is briefly discussed.

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