DOE OSTI2015
Making use of a set of detailed potential models for normal spiral galaxies, we analyze disk stellar-orbital dynamics as the structural and dynamical parameters of spiral arms (mass, pattern speed, and pitch angle) are gradually modified. With this comprehensive study of ordered and chaotic behavior, we constructed an assemblage of orbitally supported galactic models and plausible parameters for orbitally self-consistent spiral arm models. We find that to maintain orbital support for the spiral arms, the spiral arm mass, M{sub sp}, must decrease with the increase of the pitch angle, i. If i is smaller than ∼10{sup ∘}, M{sub sp} can be as large as ∼7%, ∼6%, or ∼5% of the disk mass, for Sa, Sb, and Sc galaxies, respectively. If i increases up to ∼25{sup ∘}, the maximum M{sub sp} is ∼1% of the disk mass, independent of morphological type, in this case. For values larger than these limits, spiral arms would likely act as transient features. Regarding the limits posed by extreme chaotic behavior, we find a strong restriction on the maximum plausible values of spiral arm parameters on disk galaxies beyond which chaotic behavior becomes pervasive. We find that for i smaller than ∼20{sup ∘}, ∼25{sup ∘}, or ∼30{sup ∘}, for Sa, Sb, and Sc galaxies, respectively, M{sub sp} can go up to ∼10%, of the mass of the disk. If the corresponding i is around ∼40{sup ∘}, ∼45{sup ∘}, ∼50{sup ∘}, M{sub sp} is ∼1%, ∼2%, ∼3% of the mass of the disk. Beyond these values, chaos dominates phase space, destroying the main periodic orbits and the neighboring quasiperiodic orbits.
79 ASTRONOMY AND ASTROPHYSICS↗