User:Tohline/Apps/WoodwardTohlineHachisu94
The Stability of SelfGravitating Polytropic Tori
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J. W. Woodward, J. E. Tohline, & I. Hachisu (1994; hereafter WTH94) used nonlinear numerical hydrodynamic techniques to examine the relative stability of selfgravitating, 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, Selfgravitating Disks in Protostellar Systems"
ApJ, vol. 420, pp. 247267 © American Astronomical Society  
Adopted Notation
This subsection has been drawn from an accompanying discussion that details how the linearamplitude development of nonaxisymmetric structure is often analyzed in numerical simulations.
Beginning with equation (2) of TH90 but ignoring variations in the vertical coordinate direction, the mass density is given by the expression,
<math>~\rho</math> 
<math>~=</math> 
<math>~\rho_0 \biggl[ 1 + f(\varpi)e^{i(\omega t  m\phi)} \biggr] \, ,</math> 
where it is understood that <math>~\rho_0</math>, which defines the structure of the initial axisymmetric equilibrium configuration, is generally a function of the cylindrical radial coordinate, <math>~\varpi</math>.
Using the subscript, <math>~m</math>, to identify the timeinvariant coefficients and functions that characterize the intrinsic eigenvector of each azimuthal eigenmode, and acknowledging that the associated eigenfrequency will in general be imaginary, that is,
<math>~\omega_m</math> 
<math>~=</math> 
<math>~\omega_R + i\omega_I \, ,</math> 
we expect each unstable mode to display the following behavior:
<math>~\biggl[ \frac{\rho}{\rho_0}  1 \biggr]</math> 
<math>~=</math> 
<math>~f_m(\varpi)e^{i[\omega_R t + i \omega_I t  m\phi_m(\varpi)]} </math> 

<math>~=</math> 
<math>~\biggl\{ f_m(\varpi)e^{im\phi_m(\varpi)}\biggr\} e^{i\omega_R t } \cdot e^{\omega_I t} </math> 

<math>~=</math> 
<math>~\biggl\{ f_m(\varpi)e^{i[\omega_R t + m\phi_m(\varpi)]} \biggr\} e^{\omega_I t} \, .</math> 
Adopting Kojima's (1986) notation, that is, defining,
<math>~y_1 \equiv \frac{\omega_R}{\Omega_0}  m</math> 
and 
<math>~y_2 \equiv \frac{\omega_I}{\Omega_0} \, ,</math> 
the eigenvector's behavior can furthermore be described by the expression,
<math>~\biggl[ \frac{\rho}{\rho_0}  1 \biggr]</math> 
<math>~=</math> 
<math>~\biggl\{ f_m(\varpi)e^{i[(y_1+m) (\Omega_0 t) + m\phi_m(\varpi)]} \biggr\} e^{y_2 (\Omega_0 t)} </math> 

<math>~=</math> 
<math>~\biggl\{ f_m(\varpi)e^{im[(y_1/m+1) (\Omega_0 t) + \phi_m(\varpi)]} \biggr\} e^{y_2 (\Omega_0 t)} \, .</math> 
Note that, as viewed from a frame of reference that is rotating with the mode pattern frequency,
<math>\Omega_p \equiv \frac{\omega_R}{m} = \Omega_0\biggl(\frac{y_1}{m}+1\biggr) \, ,</math>
we should find an eigenvector of the form,
<math>~\biggl[ \frac{\delta\rho}{\rho_0}\biggr]_\mathrm{rot} \equiv \biggl[ \frac{\rho}{\rho_0}  1 \biggr]e^{im\Omega_p t}</math> 
<math>~=</math> 
<math>~\biggl\{ f_m(\varpi)e^{im[\phi_m(\varpi)]} \biggr\} e^{y_2 (\Omega_0 t)} \, ,</math> 
whose relative amplitude — with a radial structure as specified inside the curly braces — is undergoing a uniform exponential growth but is otherwise unchanging.
Drawing from figure 2 of WTH94, our Figure 1, immediately below, illustrates how the behavior of each factor in this expression can reveal itself during a numerical simulation that follows the timeevolutionary development of an unstable, nonaxisymmetric eigenmode. The initial model for this depicted evolution (model O3 from Table 1 of WTH94) is a zeromass — that is, it is a PapaloizouPringle like torus — with polytropic index,<math>~n = 3</math>, and a rotationlaw profile defined by uniform specific angular momentum.
 The topleft panel shows how, at any radial location, the phase angle, <math>~\phi_1/(2\pi)</math>, for the <math>~m=1</math> eigenmode, varies with time, <math>~t/t_\mathrm{rot}</math>, where, <math>~t_\mathrm{rot} \equiv 2\pi/\Omega_0</math> is the rotation period at the density maximum;
 Using a semilog plot, the topright panel shows the exponential growth of the amplitude of three separate modes: The dominant unstable mode, displaying the largest amplitude, is <math>~m = 1</math>.
 Using a semilog plot (log amplitude versus fractional radius, <math>~\varpi/r_+</math>), the bottomleft panel displays the shape of the eigenfunction, <math>~f_1(\varpi)</math>, for the unstable, <math>~m=1</math> mode;
 The bottomright panel displays the radial dependence of the equatorialplane phase angle, <math>~\phi_1(\varpi)</math>, for the unstable, <math>~m=1</math> mode; this is what HI11 refer to as the "constant phase locus."
Figure 1 
Four panels extracted^{†} from figure 2, p. 252 of J. W. Woodward, J. E. Tohline & I. Hachisu (1994)
"The Stability of Thick, Selfgravitating Disks in Protostellar Systems"
ApJ, vol. 420, pp. 247267 © American Astronomical Society 
^{†}As displayed here, the layout of figure panels (a, b, c, d) has been modified from the original publication layout; otherwise, each panel is unmodified. 
Online Movies
Drawing from the description presented in §Va of WTH94, the early evolution of each model behaved qualitatively in a manner depicted in Figure 1, above. For the first few rotation periods, the amplitude remained quite small for all azimuthal Fourier modes — see early times in the upperright panel of Figure 1 — and there was no apparent organized behavior exhibited by the Fourier phase angles, <math>~\phi_m</math>. Then a clearly identifiable eigenfunction for either mode <math>~m = 1</math> or <math>~m = 2</math> developed out of the initially random noise, signaled by an exponential growth of the mode amplitude — see late times in the upperright panel of Figure 1 — and a periodic oscillation of <math>~\phi_m</math> — see late times in the upperleft panel of Figure 1. A clear depiction of the radially dependent (bottomleft figure panel) and azimuthally dependent (bottomright figure panel) structure of the unstable mode also emerged from the initially random noise. The bottomright panel of Figure 1 displays, specifically for the WTH94 model O3 the constant phase locus that was present at late times.
Figure 2: Animation Sequences to Supplement Figure 10 of WTH94 (click on securitylock 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: Constant phase locus diagrams — that is, "<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 Pmode, shown here as it developed in model O15 <math>~[M_d/M_c = 1; ~T/W = 0.316];</math> (b) The m = 1 Amode, shown here as it developed in model O14 <math>~[M_d/M_c = 1; ~T/W = 0.251];</math> (c) The m = 2 Imode, shown here as it developed in model E17 <math>~[M_d/M_c = 5; ~T/W = 0.256];</math> (d) The m = 2 Lmode, shown here as it developed in model E29 <math>~[M_d/M_c = 0.2; ~T/W = 0.447]\, .</math> 
The middle panel of our Figure 2 is a reproduction of Figure 10 from WTH94. It shows the constant phase locus that emerged from the noise at late times during the evolution of four models: (a) Model O15; (b) model O14; (c) model E17; and (d) model E29. In the early '90s when this set of model simulations was carried out, we saved numerical data that detailed the timeevolutionary behavior of both the radial and azimuthal structure of each model's fastest growing eigenfunction. This data allowed us to generate afterthefact, for example, plots of the constant phase locus at many different points in time to explicitly show how the azimuthally dependent eigenfunction developed out of the initial noise. Using techniques described in Tohline (2007), we transferred these plots, frame by frame, to VHS video tape so that this development could be viewed as an animation. Recently we have employed an analogtodigital converter to create digital animations from nine of these analog VHS recordings, and each of the animations has been uploaded to YouTube. (The result of these analogtodigital conversions was, unfortunately, digital animations of low fidelity. They are nevertheless informative.) Our Figure 2 displays a still image from, and provides a link to the YouTube animations that depict the timeevolutionary behavior of models O15 (upper left), O14 (upper right), E17 (lower left), and E29 (lower right); in order to play the desired YouTube video, click on the securitylock icon or the model name that accompanies the associated still image.
Links to five additional animation sequences are provided, immediately below, in our Figure 3. As is identified by the short caption accompanying each still image, these animations are from, respectively, models O13, O16, O17, O18, and O22.
Figure 3: Five Additional Animation Sequences to Supplement Table 5 of WTH94 (click on securitylock 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 
See Also
 Characteristics of Unstable Eigenvectors in SelfGravitating Tori
 W. K. M. Rice, G. Lodato, & P. J. Armitage (2005), MNRAS, 364, L5660. Investigating fragmentation conditions in selfgravitating accretion discs
This article describes 3D SPH simulations with 250,000 SPH particles in the disk and a single particle representing the central star. They address disk fragmentation in the context of rapid cooling of the disk.  J. E. Tohline (2007), Computing in Science & Engineering, vol. 9, no. 6, pp. 76  81. Scientific Visualization: A Necessary Chore … (PDF)
© 2014  2021 by Joel E. Tohline 