${{\bf S}}=0$: Christodoulou (1991) investigated disk stability, while Nusser (2002) and Knebe & Gibson (2004) explored cosmological structure formation[^1].

In this paper we present results of N-body simulations of dissipationless collapse in MOND. The simulations were performed with an original three-dimensional particle-mesh N-body code, based on the numerical MOND potential solver presented in CLN, which solves equation (\[eqMOND\]) exactly. These numerical experiments are interesting both from a purely dynamical point of view, allowing for the first time to explore the relaxation processes in MOND, and in the context of elliptical galaxy formation. In fact, the ability of dissipationless collapse at producing systems strikingly similar to real ellipticals is a remarkable success of Newtonian dynamics (e.g., van Albada 1982; Aguilar & Merritt 1990; Londrillo, Messina & Stiavelli 1991; Udry 1993; Trenti, Bertin & van Albada 2005; Nipoti, Londrillo, & Ciotti 2006, hereafter NLC06), while there have been no indications so far that MOND can work as well in this respect. Here we study the structural and kinematical properties of the end-products of MOND simulations, and we compare them with the observed scaling relations of elliptical galaxies: the Faber–Jackson (FJ) relation (Faber & Jackson 1976), the Kormendy (1977) relation, and the Fundamental 