Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mnras.416..479c&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 416, Issue 1, pp. 479-492.
Astronomy and Astrophysics
Astronomy
Galaxies: Kinematics And Dynamics, Galaxies: Spiral, Galaxies: Structure
Scientific paper
Recently it has been realized that the major structures observed in rotating disc galaxies, i.e. bars and spirals, can be supported by regular as well as by chaotic orbits. The fact that the building of a structure cannot be attributed just to quasi-periodic orbits associated with a single orbital family, creates the need to classify the trajectories of the particles in structure supporting and structure non-supporting within a time interval of interest. Our goal is to present a simple algorithm that detects and classifies the orbits which reinforce the rectangularity of the outer envelope of a bar, independently of their regular or chaotic character. Our bar is a two-dimensional (2D) response bar, formed when an external potential estimated from near-infrared observations of an early-type barred-spiral galaxy, is imposed to a set of initial conditions. For this purpose we use a method based on tracing patterns in sequences of characters, which indicate sign changes of the (Cartesian) coordinates. These sign changes occur when as integrate an orbit for a time t and we follow it in 2D subspaces of the phase space [(? etc.]. A sign change indicates crossing of an axis during the integration. In the case we describe in our paper the bar in the inner parts is supported by regular orbits following the x1 flow, while the outer envelope of the bar is supported mainly by chaotic orbits at higher energies. With our method, at a given Jacobi constant, first we assess the contribution to the local surface density of a large number of orbital segments. This is done by integrating their initial conditions for 10 pattern rotations. We depict this information on grey-scale maps. We have realized that this contribution is independent of the regular or chaotic character of the integrated orbits. Then, by analysing the arrays of sign changes we have registered during the orbital integrations, we separate the trajectories that shape the outer structure of the bar in two classes. They follow mainly boxy or/and diamond-like morphologies within the time of integration. By repeating the method at several Jacobi constants (EJ) we find that the majority of the orbits that support the morphological feature we study, i.e. the boxiness of the bar, are found in a narrow ΔEJ interval.
Boily Christian M.
Chatzopoulos S.
Patsis Panos A.
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