Global non-axisymmetric perturbation configurations in a composite disc system with an isopedic magnetic field: relation between dark matter halo and magnetic field

Abstract

We study global non‐axisymmetric stationary perturbations of aligned and unaligned logarithmic spiral configurations in an axisymmetric composite differentially rotating disc system of scale‐free stellar and isopedically magnetized gas discs coupled by gravity. The infinitely thin gas disc is threaded across by a vertical magnetic field Bz with a constant dimensionless isopedic ratio of surface gas mass density Σ(g) to Bz with G being the gravitational constant. Our exploration focuses on the relation between the isopedic ratio λ and the dark matter amount represented by a gravitational potential ratio in order to sustain stationary perturbation configurations, where is the gravitational potential of a presumed axisymmetric halo of dark matter and Φ is the gravitational potential of the composite disc matter. For typical disc galaxies, we explore relevant parameter ranges numerically. High and low λ values correspond to relatively weak and strong magnetic fields given the same gas surface mass density, respectively. The main goal of our model analysis is to reveal the relation between isopedic magnetic fields and dark matter halo in spiral galaxies with globally stationary perturbation configurations. Our results show that for stationary perturbation configurations, fairly strong yet realistic magnetic fields require a considerably larger amount of dark matter in aligned and unaligned cases than weak or moderate magnetic field strengths. We discuss astrophysical and cosmological implications of our findings. For examples, patterns and pattern speeds of galaxies may change during the course of galactic evolution. Multiple‐armed galaxies may be more numerous in the early Universe. Flocculent galaxies may represent the transitional phase of pattern variations in galaxies.

Dark matter dominated dwarf disc galaxy Segue 1

“…In spite of observational uncertainties, we may presume that Segue 1 has an unusually large ratio f calling for further observational and theoretical confirmations. In this Letter, we presume Segue 1 as a dwarf disc galaxy , apply our composite model for disc galaxies (Xiang‐Gruess, Lou & Duschl 2009, hereafter XLD) and focus on relevant aspects of this DM issue as well as the possible role of a magnetic field in its interstellar gas disc.…”