Towards the Unified Theory of Galactic Bar-Modes

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dc.creatorPolyachenko, E. V.
dc.creatorPolyachenko, V. L.
dc.date2002-12-27
dc.date.accessioned2026-07-07T02:07:01Z
dc.date.available2026-07-07T02:07:01Z
dc.descriptionThe arguments in favor of the unified formation mechanism for both slow (Lynden-Bell's) bars and common fast bars are given. This mechanism consists in a certain instability that is akin to the well-known radial orbit instability; it is caused by the mutual attraction and alignment of axes of precessing star orbits (up to now, such a way of formation was considered only for slow bars). The general theory of the low-frequency modes of a disk consisting of precessing orbits (at different angular velocities) is presented. The problem of determining these modes is reduced to the integral equations of a rather simple structure. The characteristic pattern speeds ($Ω_p$) of the low-frequency modes are of order of the mean orbit precession speeds ($\barΩ_{pr}$). The bar-modes also belong to this type of modes. The slow bars have $Ω_p \approx \barΩ_{pr}$; for the fast bars, $Ω_p$ may far exceed even the maximum precessing speed of disk orbits (however, $Ω_p$ remains to be of order of these precessing speeds). The possibility of such an excess of $Ω_p$ over $Ω_{pr}^{\max}$ is connected with the effect of ``repelling'' orbits that tend to move in the direction opposite to that they are being pushed. The preliminary analysis of the orbit precession patterns for a number of typical potentials is given. It is noted that the maximum radius of the ``attracting'' circular orbits ($r_c$) may be used as a reasonable estimate of a bar length.
dc.description19 pages
dc.identifierhttps://arxiv.org/abs/astro-ph/0212553
dc.identifierhttp://arxiv.org/abs/astro-ph/0212553
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5559
dc.subjectAstrophysics
dc.titleTowards the Unified Theory of Galactic Bar-Modes
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