User:Tohline/Apps/WoodwardTohlineHachisu94

The Stability of Self-Gravitating Polytropic Tori

J. W. Woodward, J. E. Tohline, & I. Hachisu (1994; hereafter WTH94) used nonlinear numerical hydrodynamic techniques to examine the relative stability of self-gravitating, polytropic tori toward the development of nonaxisymmetric structure. The following pair of tables list key properties of the set of model tori that were examined: Table 5 gives characteristics of the initial models and Table 6 presents results ascertained from the numerical stability analyses.

Table extracted from J. W. Woodward, J. E. Tohline & I. Hachisu (1994) "The Stability of Thick, Self-gravitating Disks in Protostellar Systems" ApJ, vol. 420, pp. 247-267 © American Astronomical Society

Online Movies

Figure 1: Animation Sequences to Supplement Figure 10 of WTH94 (click on security-lock icon or caption model name to go to YouTube)
Table 5, Model O15		Table 5, Model O14
Table 5, Model E17		Table 5, Model E29
Caption to Fig. 10 from WTH94:  "<math>~\phi_m - r</math>" diagrams illustrating the azimuthal structure of the four specific eigenmodes that were found to be dynamically unstable in our modeled disks.  (a) The m = 1 P-mode, shown here as it developed in model O15 <math>~[M_d/M_c = 1; ~T/|W| = 0.316];</math>  (b) The m = 1 A-mode, shown here as it developed in model O14 <math>~[M_d/M_c = 1; ~T/|W| = 0.251];</math>  (c) The m = 2 I-mode, shown here as it developed in model E17 <math>~[M_d/M_c = 5; ~T/|W| = 0.256];</math>  (d) The m = 2 L-mode, shown here as it developed in model E29 <math>~[M_d/M_c = 0.2; ~T/|W| = 0.447]\, .</math>

Figure 2: Five Additional Animation Sequences to Supplement Table 5 of WTH94 (click on security-lock icon or caption model name to go to YouTube)
Table 5, Model O13	Table 5, Model O16	Table 5, Model O17	Table 5, Model O18	Table 5, Model O22

 

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