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The stability of accretion tori. I. Long-wavelength modes of slender tori

Goldreich, Peter and Goodman, Jeremy and Narayan, Ramesh (1986) The stability of accretion tori. I. Long-wavelength modes of slender tori. Monthly Notices of the Royal Astronomical Society, 221 (2). pp. 339-364. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20130313-071925944

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Abstract

We elucidate the inviscid instabilities of an isentropic torus found previously by Papaloizou & Pringle. The torus is a polytrope of index, n, and has a small ratio of minor radius, ɑ, to orbital radius, r_0. In equilibrium it rotates on cylinders with angular velocity profile Ω,∝r^(-q). Linear modes are proportional to exp i(mØ-wt). For small β≡mα/r_0 , we justify the use of height-averaged equations by appealing to approximate vertical hydrostatic equilibrium. The effective polytropic index for the resulting two-dimensional problem is N≡n+½; thus an incompressible torus in three dimensions behaves compressibly in two. Height averaged modes obey an ordinary differential equation, which we solve numerically to obtain the growth rate as a function of q, n, and β. The error made in predicting the growth rate of the actual three-dimensional system is small everywhere along the principal branch even for β~0.5, and is less than 1 per cent for the fastest-growing mode. We analytically solve the artificial case n=-½, which is two-dimensionally incompressible, and show that it has all the qualitative features of the general case, except that it does not have a resonance at corotation. In the general case, with n>-½ and q<2, the corotation resonance absorbs energy and angular momentum, so the growing and decaying modes do not occur in complex-conjugate pairs. We solve a second special case, namely n=2-q=0, almost analytically in three dimensions, without height-averaging. Papaloizou & Pringle asserted that this system is stable but we show that there is an unstable mode for small β just as in the other systems. In fact this principal unstable branch, with corotation at the pressure maximum, is qualitatively the same for all n and is essentially independent both of compressibility and of the gradient in vorticity per unit surface density. Thus the modes are not sonic, nor are they similar to those of the Kelvin-Helmholtz instability. Instead they are composed of two edge waves, akin to surface waves in water although modified by shear and rotation, coupled across a forbidden region around corotation.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://adsabs.harvard.edu/abs/1986MNRAS.221..339GADSArticle
ORCID:
AuthorORCID
Narayan, Ramesh0000-0002-1919-2730
Additional Information:© 1986 Royal Astronomical Society. Accepted 1986 February 5. Received 1986 February 5; in original form 1985 November 11. We thank Roger Blandford for encouragement and advice and John Papaloizou and Jim Pringle for sending us their papers far in advance of publication. We note that Omar Blaes and Wolfgang Glatzel have independently derived many of the results reported in this paper. Our research was supported in part by the NSF through grants AST83-13725 and AST82-13001.
Funders:
Funding AgencyGrant Number
NSFAST83-13725
NSFAST82-13001
Issue or Number:2
Record Number:CaltechAUTHORS:20130313-071925944
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130313-071925944
Official Citation:The stability of accretion tori. I - Long-wavelength modes of slender tori Goldreich, P.; Goodman, J.; Narayan, R. Monthly Notices of the Royal Astronomical Society vol. 221, July 15, 1986, p. 339-364
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:37482
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:13 Mar 2013 14:55
Last Modified:02 Nov 2019 20:07

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