Rotation curves of rotating Galactic Bose-Einstein condensate dark matter halos

Abstract

We present the dynamics of rotating Bose Condensate galactic dark matter halos, made of an ultralight spinless boson. We restrict to the case of adding axisymmetric rigid rotation to initially spherically symmetric structures and show there are three regimes: i) small angular momentum, that basically retains the drawbacks of spherically symmetric halos related to compactness and failure at explaining galactic RCs, ii) an intermediate range of values of angular momentum that allow the existence of long-lived structures with acceptable RC profiles, and iii) high angular momentum, in which the structure is dispersed away by rotation. We also present in detail the new code used to solve the Gross-Pitaevskii Poisson system of equations in three dimensions.

Evolution and dynamical properties of Bose-Einstein condensate dark matter stars

“…Rotating BEC halos were also discussed [19]. The possibility that the superfluid interior of compact astrophysical objects may be at least partially in the form of a BEC [20], and the possible presence of a boson condensate in stars and their stability properties [21] were also investigated.…”

Scalar field (wave) dark matter

“…Moreover, there is particular interest in finding equilibrium configurations of the system of equations that describe the field (Einstein-Klein-Gordon system) and of its weak field approximation (Schrödinger-Poisson(SP) system), different authors have obtained solutions interpreted as boson stars or later as dark matter halos showing agreement with rotation curves in galaxies and velocity dispersion profiles in dwarf spheroidal galaxies 4,18,27,36,38,39,43,55,56 . So far the large and small scales observations are well described with the small mass and thus has been taken as a prefered value but the precise values of the mass and self-interaction parameters are still uncertain, tighter constraints can come from numerical simulations 62 and modeling of large galaxy samples.…”

“…Depending on the number density of bosons populating the excited states we can have different fates for the halos 58 . On the other hand, including rotation in the halo might be needed, in fact, 27 have included rotation to axis-symmetric halos in the condensed state and show that it can lead to the flattening of the RCs, other works have also included rotation but in the context of MSHs in asymmetric configurations 9 , both studies suggest that rotation is a relevant ingredient in halo modeling, in fact it should be, in the end we observed rotation in galaxies embedded in dark halos. However, we require more detail studies to assess the goodness of the agreement with a large sample of galaxies, especially because there ara several surveys underway (e.g.…”

Rotation curves of ultralight BEC dark matter halos with rotation

“…On the one hand, even though excited states are unstable, the superposition of ground and excited states turned out to be stable and show appealing galactic RCs [26]. On the other hand, some rotation has been added to ground state configurations that disperse away the density of the condensate and show also appealing RCs [27]. The possibility that BEC dark matter halos may have rotation has been pointed out before in [28], where spheroid and ellipsoid analytic solutions to the GPP system with rotation are studied as rotating BEC dark matter halos in various scenarios, and the results particularly focus on the possibility of vortex formation, but little is said about the comparison with observations, say RCs.…”

“…What we do in this paper is to try to answer the question of whether the long-lived rotating or spherical configurations in [27] are capable of fitting observed RCs. For this we focus on a sample of dark matter dominated LSB galaxies, for which, as a first approximation, luminous matter would not contribute significantly to the total mass of the system and thus behave as test particles.…”