Table 14: Application of the coronal loop models of Aschwanden & Schrijver (2002) to the innermost three shells of 2A 0335+096. M₁₃ is the total cluster mass in $10^{13}~M_{\hbox{$\odot$ }}$ within the radius R (kpc), for which we take the average radius of the shell. $\overline {\rho _l}/\rho _{{\rm tot}}$ is the average mass density of the loops divided by the total mass density of the cluster (including dark matter etc.). The total mass density profile was taken from Ettori et al. (2002). In this table, f is the volume filling factor of the loops.
shell 1 2 3

M₁₃ 0.0025 0.07 0.5

R (kpc) 14 43 86

$\Gamma$ 4-6 7-40 1-100

L (kpc) 3.6f^0.5 11f^0.5 44f^0.5

$\overline {\rho _l}/\rho _{{\rm tot}}$ 0.64f^0.5 0.33f^0.5 0.15f^0.5

N 7-11 f^0.5 14-70 f^0.5 12-500 f^0.5

**Table 14:** Application of the coronal loop models of Aschwanden & Schrijver (2002) to the innermost three shells of 2A 0335+096. M₁₃ is the total cluster mass in $10^{13}~M_{\hbox{$\odot$ }}$ within the radius R (kpc), for which we take the average radius of the shell. $\overline {\rho _l}/\rho _{{\rm tot}}$ is the average mass density of the loops divided by the total mass density of the cluster (including dark matter etc.). The total mass density profile was taken from Ettori et al. (2002). In this table, f is the volume filling factor of the loops.
shell	1	2	3
M₁₃	0.0025	0.07	0.5
R (kpc)	14	43	86
$\Gamma$	4-6	7-40	1-100
L (kpc)	3.6f^0.5	11f^0.5	44f^0.5
$\overline {\rho _l}/\rho _{{\rm tot}}$	0.64f^0.5	0.33f^0.5	0.15f^0.5
N	7-11 f^0.5	14-70 f^0.5	12-500 f^0.5

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