View source for User:Tohline/Appendix/Ramblings/Hadley and Imamura Supplementary Database

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=Supplementary Dataset Generated by Hadley &amp; Imamura Collaboration=
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Using numerical hydrodynamic techniques, the [[#See_Also|Hadley &amp; Imamura collaboration]] &#8212; see especially [http://adsabs.harvard.edu/abs/2011Ap%26SS.334....1H Paper I] and [http://adsabs.harvard.edu/abs/2014Ap%26SS.353..191H Paper II] &#8212; has studied the dynamical development of nonaxisymmetric instabilities in toroidal configurations that have a range of "star-to-disk" mass ratios and a wide variety of (initially axisymmetric) geometric structures.  We have begun to analyze the results of these numerical simulations in the context of what is known, analytically, about normal modes of oscillation and nonaxisymmetric instabilities in [[User:Tohline/Apps/PapaloizouPringleTori#Massless_Polytropic_Tori|''massless'' Papaloizou-Pringle tori]].  On the analytic side, our focus has been on the very informative stability analysis published by [http://adsabs.harvard.edu/abs/1985MNRAS.216..553B Blaes (1985)].


This brief appendix is provided primarily to support our accompanying discussion of the "[[User:Tohline/Apps/ImamuraHadleyCollaboration#Characteristics_of_Unstable_Eigenvectors_in_Self-Gravitating_Tori|Characteristics of Unstable Eigenvectors in Self-Gravitating Tori]];" especially the [[User:Tohline/Apps/ImamuraHadleyCollaboration#Comparison_with_Results_from_the_Imamura_.26_Hadley_Collaboration|subsection of that chapter]] in which some results from the Hadley &amp; Imamura collaboration are directly compared to the analytic analysis by [http://adsabs.harvard.edu/abs/1985MNRAS.216..553B Blaes (1985)].  In addition to the relatively small number of individual models whose unstable eigenvectors have been described in the published literature &#8212; see especially the [[#See_Also|three papers listed below]] &#8212; Hadley and Imamura have stored digital results from a very large number of model simulations in an [http://pages.uoregon.edu/khadley/ online ''Stardisks'' repository].  We greatly appreciate being granted permission (explicitly by K. Z. Hadley) to access this data repository and to post this link so that other researchers may study the accumulated data.

=See Also=
* Hadley &amp; Imamura collaboration:
** <font color="red"><b>Paper I</b></font>:   [http://adsabs.harvard.edu/abs/2011Ap%26SS.334....1H K. Hadley &amp; J. N. Imamura (2011, ''Astrophysics and Space Science'', 334, 1-26)], "Nonaxisymmetric instabilities in self-gravitating disks. &nbsp; I. Toroids" &#8212; In this paper, Hadley &amp; Imamura perform linear stability analyses on fully self-gravitating toroids; that is, there is no central point-like stellar object and, hence, <math>~M_*/M_d = 0.0</math>.
** <font color="red"><b>Paper II</b></font>:  [http://adsabs.harvard.edu/abs/2014Ap%26SS.353..191H K. Z. Hadley, P. Fernandez, J. N. Imamura, E. Keever, R. Tumblin, &amp; W. Dumas (2014, ''Astrophysics and Space Science'', 353, 191-222)], "Nonaxisymmetric instabilities in self-gravitating disks. &nbsp; II. Linear and quasi-linear analyses" &#8212; In this paper, the Imamura &amp; Hadley collaboration performs "an extensive study of nonaxisymmetric global instabilities in thick, self-gravitating star-disk systems creating a large catalog of star/disk systems &hellip; for star masses of <math>~0.0 \le M_*/M_d \le 10^3</math> and inner to outer edge aspect ratios of <math>~0.1 < r_-/r_+ < 0.75</math>."
** <font color="red"><b>Paper III</b></font>:  [http://adsabs.harvard.edu/abs/2015Ap%26SS.359...10H K. Z. Hadley, W. Dumas, J. N. Imamura, E. Keever, &amp; R. Tumblin (2015, ''Astrophysics and Space Science'', 359, article id. 10, 23 pp.)], "Nonaxisymmetric instabilities in self-gravitating disks. &nbsp; III. Angular momentum transport" &#8212; In this paper, the Imamura &amp; Hadley collaboration carries out nonlinear simulations of nonaxisymmetric instabilities found in self-gravitating star/disk systems and compares these results with the linear and quasi-linear modeling results presented in Papers I and II.



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