On the eccentricity of self-gravitating circumstellar disks in eccentric binary systems

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Volume 508 / No 3 (December IV 2009)

A&A, 508 3 (2009) 1493-1502

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Table 1:

Location of the mean motion resonances within the circumprimary disk up to order 10.
i	j	a (AU)
3	1	12.89
10	3	12.01
7	2	11.63
4	1	10.64
9	2	9.84
5	1	9.17
6	1	8.12
7	1	7.32
8	1	6.70
9	1	6.19

The critical argument is of the type $i \lambda_{\rm c} - j \lambda_{\rm g} - n \varpi_{\rm c} -m \varpi_{\rm g}$ where $\lambda_{\rm c}$ is the true anomaly of the companion star and $\lambda_{\rm g}$ that of the gas while $\varpi_{\rm g}$ is the perihelion longitude of the gas. $\varpi_{\rm c}$ is the perihelion longitude of the star which is constant in our simulations.

Source LaTeX | All tables | In the text

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