Difference between revisions of "User:Tohline/Appendix/Ramblings/Saturn"
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<th align="center" colspan="3">FIGURE 3: Nonlinear-Amplitude Distortions that Develop in Three Separate Model Evolutions</th> | |||
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<th align="center">Evolution A</th> | |||
<th align="center">Evolution B</th> | |||
<th align="center">Evolution C</th> | |||
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The following discussion has largely been extracted from §3.1.4 of [https://ui.adsabs.harvard.edu/abs/2017ApJS..229...27M/abstract MFSCFEDT (2017)]: | |||
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<font color="green">In §4 of their paper, [https://ui.adsabs.harvard.edu/abs/2006ApJ...643..381D/abstract MFTD (2007)] point out that in the vicinity of the accretor some of the models developed nonlinear-amplitude "equatorial distortions with [azimuthal mode numbers] <math>~6 \ge m \ge 3</math>."</font> As is illustrated by the trio of images displayed in the bottom row of Figure 3, above, at a certain point (or points) in each of these binary mass-transfer evolutions <font color="green">… the disk surrounding the accretor has a triangular shape …</font> This trio of ''triangular shaped'' images come from, respectively, evolutionary times: (A, B, C) = (15.3, 17.50, 24.33), as measured in terms of initial orbital periods. | |||
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=Related Discussions= | =Related Discussions= | ||
Revision as of 23:58, 12 July 2019
Saturn
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Hexagon Storm
Image on the Right: obtained from this NASA/JPL site; image on the Left: obtained from this NASA Newsletter. See also the wikipedia page titled, Saturn's hexagon.
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Post Cassini
Binary Mass-Transfer
Several key references:
- [Paper DMTF (2006)] M. C. R. D'Souza, P. M. Motl, J. E. Tohline & J. Frank (2006), ApJ, 643, p. 381: Numerical Simulations of the Onset and Stability of dynamical Mass Transfer in Binaries
- [Paper MFTD (2007)] P. M. Motl, J. Frank, J. E. Tohline & M. C. R. D'Souza (2007), ApJ, 670, p. 1314: The Stability of Double White Dwarf Binaries Undergoing Direct-Impact Accretion
- [Paper MFSCFEDT (2017)] P. M. Motl, J. Frank, J. Staff, G. C. Clayton, C. L. Fryer, W. Even, S. Diehl & J. E. Tohline (2017), ApJSuppl., Vol. 229, Issue 2, article id. 27, 41 pp.: A Comparison of Grid-based and SPH Binary Mass-transfer and Merger Simulations
| FIGURE 3: Nonlinear-Amplitude Distortions that Develop in Three Separate Model Evolutions | ||
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| Evolution A | Evolution B | Evolution C |
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MFTD (2007) |
MFSCFEDT (2017) |
MFSCFEDT (2017) |
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| †The evolution identified here as Model Q0.5P_G1 was first discussed in §5.2 of DMTF (2006), wherein it was identified as Model Q0.5-Da; the caption to Figure 7 of that paper contains a link to an (mpeg_file = video3-2.mpg) animation that presents a 3D rendering of this model's evolution. | ||
The following discussion has largely been extracted from §3.1.4 of MFSCFEDT (2017):
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In §4 of their paper, MFTD (2007) point out that in the vicinity of the accretor some of the models developed nonlinear-amplitude "equatorial distortions with [azimuthal mode numbers] <math>~6 \ge m \ge 3</math>." As is illustrated by the trio of images displayed in the bottom row of Figure 3, above, at a certain point (or points) in each of these binary mass-transfer evolutions … the disk surrounding the accretor has a triangular shape … This trio of triangular shaped images come from, respectively, evolutionary times: (A, B, C) = (15.3, 17.50, 24.33), as measured in terms of initial orbital periods. |
Related Discussions
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