In an effort to better understand the formation and evolution of barred galaxies, we have examined the properties of equatorial orbits in the effective potential of one specific model of a rapidly rotating, steady-state gas-dynamical bar that has been constructed via a self-consistent hydrodynamical simulation. At a given value of the Jacobi constant, roughly half of all test particles (stars) ...

Stellar dynamics is almost unreasonably well suited for an implementation in terms of special-purpose hardware. Unlike the case of molecular dynamics, stellar dynamics deals exclusively with a long-range force, gravity, which leads to a computational cost scaling as the square of the number of stars involved. While special tricks can lead to a reduction of this cost from ∼ N2 to ∼ N logN in the...

I present a discussion of fundamental stellar parameters and their observational determination in the context of interferometric measurements with current and future optical/infrared interferometric facilities. Stellar parameters and the importance of their determination for stellar physics are discussed. One of the primary uses of interferometry in the field of stellar physics is the measureme...

Context. People usually estimate the ages and metallicities of dominating stellar populations of galaxies without current star formation, e.g., early type galaxies, by comparing the observed absorption line indices or colors to predictions of some simple stellar populations, which have only a star burst or have star bursts within a short period. However, some studies show that there are recent ...

We define the manifold of configurations to be quotient set k points in Euclidean space identified under congruence, and prove that compact subsets ℝd, d≥2, large Hausdorff dimension have a non-null them. Our method simplifies previous work achieves better dimensional threshold.

Abstract We examine the static structure configurations and radial stability of compact stars within context f(R, T) gravity, with R T standing for Ricci scalar trace energy-momentum tensor, respectively. Considering T)=R+2? functional form, ? being a constant, we derive corresponding hydrostatic equilibrium equation modified Chandrasekhar's pulsation equation. The mass-radius relations mode fr...