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Widths of Lindblad Resonances in Galaxies: Origin of the Hole in the Gas Disk of the Milky Way

Published online by Cambridge University Press:  12 April 2016

Leonid Marochnik ,
Roald Sagdeev  and
Daniel Usikov
Leonid Marochnik
Affiliation:
Computer Sciences Corporation, Lanham, Maryland, 20706
Roald Sagdeev
Affiliation:
Department of Physics, University of Maryland, College Park, Maryland, 20742-3280
Daniel Usikov
Affiliation:
Department of Physics, University of Maryland, College Park, Maryland, 20742-3280

Abstract

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It is shown that slopes of p(R) = Ω(R) ± κ(R)/m curves at Lindblad resonances determine the widths of resonance regions. The ability of galactic disks to respond to torques exerted at ILRs by perturbers (bar, density wave, galaxy-satellite, etc.) is determined by the widths of inner Lindblad resonances (ILRs). Widths of ILRs vary along the Hubble sequence of normal and barred galaxies. Galaxies having the bulge to disk ratio of masses and radii similar to the Milky Way could have wide ILRs if they are formed at the region of 2-4 kpc from their centers. A wide range of possible perturbers with pattern speeds 4≤ Ωp ≤ 26 km s≤1 kpc−1 could excite an ILR at this region of the Milky Way. Probably, the ILR of Milky Way’s grand design is located in the same region. The hole in the galactic H2 disk is also located in this region. The mechanism responsible for the origin of this hole could be similar to that opening gaps in planetary rings.

Type
Part IX. The Galaxy as a Barred Spiral
Information
International Astronomical Union Colloquium , Volume 157: Barred Galaxies , 1996 , pp. 540 - 544
Copyright
Copyright © Astronomical Society of the Pacific 1996

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