Table 7: Parameters of the dust models for WR 102ka and WR 102c. The ``inner part'' model is designed to reproduce the SED as observed through the aperture of the Spitzer IRS spectrograph, while the emission from the ``outer part'' model matches the SED constrained by the MSX photometric measurements (see text for details).
  WR 102ka WR 102c
Input parameter        
$a_{\rm {min}}~[\mbox{$\mu$ m}]$ 0.001 0.005
$a_{\rm {max}}~[\mbox{$\mu$ m}]$ 7.50 10.0
Input parameter inner part outer part inner part outer part
$T_{1}~[\rm {K}]$ 200 150 175 130
Y 2 3 2 3
$\tau_{\rm V}$ $1.2\times 10^{-3}$ $1.7\times 10^{-2}$ $8.1\times 10^{-3}$ $1.5\times 10^{-1}$
Inferred parameter inner part outer part inner part outer part
$r_1~[\rm {pc}]$ 0.06 0.12 0.07 0.15
$r_2~[\rm {pc}]$ 0.12 0.36 0.15 0.45
$\tau_{20~\mbox{$\mu$ m}}$ $1.6\times 10^{-4}$ $2.2\times 10^{-3}$ $1.2\times 10^{-3}$ $1.3\times 10^{-2}$
$M_{\rm {dust}}~[\mbox{$M_\odot$ }]$ $6\times 10^{-5}$ $5\times 10^{-3}$ $7\times 10^{-4}$ $8\times 10^{-2}$


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