2017/03/16 by Neda Ghafourian, Mahmood Roshan · 12 citations
Physics and Astronomy · #Astronomy #Astrophysics #Bar (unit) #Classical mechanics #Context (archaeology) #Cosmology #Cosmology and Gravitation Theories #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #Instability #Mathematical physics #Newtonian fluid #Newtonian limit #Physics #Quantum mechanics #Sigma #Spiral galaxy #Stellar, planetary, and galactic studies #astro-ph.GA #gr-qc
paper · pdf · doi:10.1093/mnras/stx661
published in Monthly Notices of the Royal Astronomical Society 468(4), 4450-4464 (Oxford University Press) · 16 pages, a reference added, few typos fixed, accepted version in MNRAS
openalex publication_date 2017/03/16 · arxiv created 2017/03/17 · openalex created_date 2017/04/07 · arxiv updated 2017/05/17 · openalex updated_date 2026/08/05
Using N-body simulations, we study the global stability of a self-gravitating disc in the context of modified gravity (MOG). This theory is a relativistic scalar–tensor–vector theory of gravity and it is presented to address the dark matter problem. In the weak field limit, MOG possesses two free parameters α and μ0, which have already been determined using the rotation curve data of spiral galaxies. The evolution of a stellar self-gravitating disc and, more specifically, the bar instability in MOG are investigated and compared to a Newtonian case. Our models have exponential and Mestel-like surface densities as Σ ∝ exp (−r/h) and Σ ∝ 1/r. It is found that, surprisingly, the discs are more stable against the bar mode in MOG than in Newtonian gravity. In other words, the bar growth rate is effectively slower than the Newtonian discs. Also, we show that both free parameters (i.e. α and μ0) have stabilizing effects. In other words, an increase in these parameters will decrease the bar growth rate.