Table 3: CO model results for the Mira sample.

Source		 P L 1 $L_{\rm d}/L_{*}$ T* $T_{\rm d}$ D $v_{\rm e}$ $\dot{M}$ $r_{\rm p}$ 2 h $\chi^2_{\rm red}$ N
  [days] [$L_{\odot }$]   [K] [K] [pc] [km s-1] [10 $^{-6}~M_\odot$ yr-1] [1016 cm]      

TX Cam		 557 8400 0.26 1800 460 380 18.5 7 8.7 1.5 0.5 4
R Cas 431 6500 0.06 2100 530 220 10.5 1.3 4.0 1.1 1.0 4
R Hya 388 5800 0.03 2300 580 150 7.0 0.3 2.0 0.5   1
R Leo 313 4600 0.02 2100 570 130 6.0 0.2 1.7 0.6 0.4 3
GX Mon 527 8000 0.38 1500 380 540 18.7 40 24.0 0.5 2.4 4
WX Psc 660 10000 0.85 920 400 600 19.3 10 11.4 0.4 6.6 4
IK Tau 500 7500 0.46 1500 500 250 18.5 30 20.5 0.3 0.4 4
IRC+10365 500 7500 0.26 1600 430 750 16.2 30 23.8 0.5 2.2 2
IRC-10529 680 10400 0.17 1000 410 270 12.0 2.5 5.8 0.1 1.6 4
IRC-30398 575 8700 0.24 2000 480 390 16.0 6 8.2 0.5 0.1 2
IRC+40004 750 11500 0.44 1700 400 410 18.0 6 8.6 0.5 2.4 2
IRC+50137 629 9600 0.57 1300 310 410 17.0 10 10.7 0.1 4.2 3
1 Derived from a period-luminosity relation.
2 The CO photodissociation radius.

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