Statistics – Computation
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20114606y&link_type=abstract
American Astronomical Society Meeting 201, #146.06; Bulletin of the American Astronomical Society, Vol. 35, p.572
Statistics
Computation
Scientific paper
Recent high resolution radio (OVRO) and optical (HST) observations have revealed the inner most spiral structure of spiral-bar galaxy NGC5248 (Jogee et al 2002, ApJ, 570,L55 ; Jogee et al 2002, ApJ, 575, 156). The spiral structure of that galaxy has been interpreted as waves driven by its major bar at the outer inner Lindblad resonance (OILR) with galacto-centric distance equal to 2.0 kpc in the 2002 paper quoted above. Associated with the OILR, there is an inner inner Lindblad resonance (IILR) at .375 kpc. In another case, a second OILR at .2 kpc is invoked. Here we use both the analytic method and numerical simulations to study the the dynamics of the same galaxy, with basically the same rotation. Although our result supports the general conclusion of theirs, i.e., the spiral structure is excited by the major bar of the system, there are significant differences between the two studies. The rotation rate of the bar is lower in our case, such that the OILR is located at 3.0! kpc and the IILR is closer to the center, if it exists at all. However, arguing from the points of the disk thickness, the density gradient, and the self-gravitation of the disk, we believe it is effectively non-existing. We also find the self-gravitation of the gas disk initially is not important. It becomes locally important when the gas mass accumulates toward the center as the disk evolves. We carry out the computations in both the non-linear asymptotic theory and the full gas-dynamic equations, to check on each other until satisfactory results are reached. Finally we compare our results with the observations. The work is in part supported by a grant from National Science Council, ROC.
Yang Changchun
Yen Chun-Chen
Yuan Changhe
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